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<ri:Resource created="2010-10-04T09:18:29Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>31 Com radial velocities</title><shortName>J/A+A/520/A52</shortName><identifier>ivo://CDS.VizieR/J/A+A/520/A52</identifier><altIdentifier>doi:10.26093/cds/vizier.35200052</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Strassmeier K.G.</name></creator><creator><name>Granzer T.</name></creator><creator><name>Kopf M.</name></creator><creator><name>Weber M.</name></creator><creator><name>Kueker M.</name></creator><creator><name>Reegen P.,Rice J.B.</name></creator><creator><name>Matthews J.M.</name></creator><creator><name>Kuschnig R.</name></creator><creator><name>Rowe J.F.</name></creator><creator><name>Guenther D.B.,Moffat A.F.J.</name></creator><creator><name>Rucinski S.M.</name></creator><creator><name>Sasselov D.</name></creator><creator><name>Weiss W.W.</name></creator><date role="Updated">2017-07-03T14:25:20Z</date><date role="Created">2010-10-04T09:18:29Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>giant-stars</subject><subject>radial-velocity</subject><description>The single rapidly-rotating G0 giant 31 Comae has been a puzzle because of the absence of photometric variability despite its strong chromospheric and coronal emissions. As a Hertzsprung-gap giant, it is expected to be at the stage of rearranging its moment of inertia, hence likely also its dynamo action, which could possibly be linked with its missing photospheric activity. Our aim is to detect photospheric activity, obtain the rotation period, and use it for a first Doppler image of the star's surface. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Obs</name><description>Observation date</description><unit>s</unit><ucd>time.epoch;obs</ucd><flag>nullable</flag></column><column><name>HJD</name><description>Heliocentric Julian date of observation</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>RV</name><description>Radial velocity</description><unit>km/s</unit><ucd>phys.veloc;pos.heliocentric</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_RV</name><description>rms uncertainty on RV</description><unit>km/s</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column></table><table><name>J/A+A/520/A52/table3</name><description>KPNO radial velocities</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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