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<ri:Resource created="2002-07-13T22:57:00Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" 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/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd 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>VI Photometry and Variables in NGC 3201</title><shortName>J/AJ/123/279</shortName><identifier>ivo://CDS.VizieR/J/AJ/123/279</identifier><altIdentifier>doi:10.26093/cds/vizier.51230279</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>von Braun K.</name></creator><creator><name>Mateo M.</name></creator><date role="Updated">2023-04-06T16:50:48Z</date><date role="Created">2002-07-13T22:57:00Z</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>globular-star-clusters</subject><subject>eclipsing-binary-stars</subject><subject>ccd-photometry</subject><subject>variable-stars</subject><description>The Globular Cluster NGC 3201 was monitored for the existence of variable stars with 16.5&lt;V&lt;20 and 0.2days&lt;period&lt;5days. The files v*.dat contain time-series photometry data in V and I for the 14 variables detected in the field of NGC 3201. Only V6 (a blue straggler contact binary) is a member of the cluster. Due to its low-latitude position, interstellar extinction is present across the field of the cluster. The file phot.dat contains VI photometry data on the monitored stars. These data are NOT corrected for extinction. The variables V7, V8, and V9 were discovered during a follow-up observing run with a different telescope and therefore do not lie in the field covered by phot.dat. 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