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<ri:Resource created="2002-11-29T21:24:10Z" 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>Velocity field in the Local Group</title><shortName>J/A+A/393/57</shortName><identifier>ivo://CDS.VizieR/J/A+A/393/57</identifier><altIdentifier>doi:10.26093/cds/vizier.33930057</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Terry J.N.</name></creator><creator><name>Paturel G.</name></creator><creator><name>Ekholm T.</name></creator><date role="Updated">2002-11-29T20:25:35Z</date><date role="Created">2002-11-29T21:24:10Z</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>galaxies</subject><subject>catalogs</subject><subject>radial-velocity</subject><description>Pratton, Melott and McKee (1997ApJ...479L..15P) showed that the velocity field around clusters could generate an apparent distortion that appears as tangential structures or radial filaments. In the present paper we determine the parameters of the Peebles' model (1976ApJ...205..318P) describing infall of galaxies onto clusters with the aim of testing quantitatively the amplitude of this distortion. The distances are determined from the concept of sosie galaxies (Paturel, 1994A&amp;A...289..711P) using 21 calibrators for which the distances were recently calculated from two independent Cepheid calibrations. 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