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<ri:Resource created="2005-03-02T22:16:24Z" 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>Cepheids BVRIJHK dereddened magnitudes</title><shortName>J/A+A/428/587</shortName><identifier>ivo://CDS.VizieR/J/A+A/428/587</identifier><altIdentifier>doi:10.26093/cds/vizier.34280587</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Kervella</name></creator><creator><name>P.</name></creator><creator><name>Bersier</name></creator><creator><name>D.</name></creator><creator><name>Mourard</name></creator><creator><name>D.</name></creator><creator><name>Nardetto</name></creator><creator><name>N.</name></creator><creator><name>Fouque</name></creator><creator><name>P.,Coude du Foresto</name></creator><creator><name>V.</name></creator><date role="Updated">2017-10-13T15:41:18Z</date><date role="Created">2005-03-02T22:16:24Z</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>variable-stars</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>stellar-radii</subject><description>The recent VINCI/VLTI observations presented in Paper I (Kervalla et al., 2004A&amp;A...416..941K) have nearly doubled the total number of available angular diameter measurements of Cepheids. Taking advantage of the significantly larger color range covered by these observations, we derive in the present paper high precision calibrations of the surface brightness-color relations using exclusively Cepheid observations. These empirical laws allow to determine the distance to Cepheids through a Baade-Wesselink type technique. The least dispersed relations are based on visible-infrared colors, for instance FV(V-K)=-0.1336+/-0.0008(V-K)+3.9530+/-0.0006. The convergence of the Cepheid (this work) and dwarf stars (Kervella et al. 2004) visible-infrared surface brightness-color relations is strikingly good. 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