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<ri:Resource created="2008-05-06T22:40:31Z" 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>Radial velocities in A2163</title><shortName>J/A+A/481/593</shortName><identifier>ivo://CDS.VizieR/J/A+A/481/593</identifier><altIdentifier>doi:10.26093/cds/vizier.34810593</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Maurogordato S.</name></creator><creator><name>Cappi A.</name></creator><creator><name>Ferrari C.</name></creator><creator><name>Benoist C.</name></creator><creator><name>Mars G.</name></creator><creator><name>Soucail G.,Arnaud M.</name></creator><creator><name>Pratt G.W.</name></creator><creator><name>Bourdin H.</name></creator><creator><name>Sauvageot J-L.</name></creator><date role="Updated">2017-10-27T14:23:54Z</date><date role="Created">2008-05-06T22:40:31Z</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>galaxy-clusters</subject><subject>redshifted</subject><subject>radial-velocity</subject><description>A2163 is among the richest and most distant Abell clusters, presenting outstanding properties in different wavelength domains. X-ray observations have revealed a distorted gas morphology and strong features have been detected in the temperature map, suggesting that merging processes are important in this cluster. However, the merging scenario is not yet well-defined. We have undertaken a complementary optical analysis, aiming to understand the dynamics of the system, to constrain the merging scenario and to test its effect on the properties of galaxies. 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