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<ri:Resource created="2013-06-21T15:55:19Z" 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>Galactic and Magellanic Cloud Cepheids distance</title><shortName>J/A+A/550/A70</shortName><identifier>ivo://CDS.VizieR/J/A+A/550/A70</identifier><altIdentifier>doi:10.26093/cds/vizier.35500070</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Groenewegen M.A.T.</name></creator><date role="Updated">2018-01-04T08:22:10Z</date><date role="Created">2013-06-21T15:55:19Z</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>milky-way-galaxy</subject><subject>magellanic-clouds</subject><subject>variable-stars</subject><subject>stellar-distance</subject><description>The metallicity dependence of the Cepheid period-luminosity (PL) relation is of importance in establishing the extragalactic distance scale. The aim of this paper is to investigate the metallicity dependence of the PL relation in V and K, based on a sample of 128 Galactic, 36 Large Magellanic Cloud (LMC), and 6 Small Magellanic Cloud (SMC) Cepheids with individual Baade-Wesselink (BW) distances (some of the stars also have an Hubble Space Telescope (HST) based and Hipparcos parallax or are in clusters) and individually determined metallicities from high-resolution spectroscopy. Literature values of the V-band, K-band, and radial velocity data were collected for the sample of Cepheids. Based on a (V-K) surface-brightness relation and a projection factor, distances were derived from a BW analysis. Since 2008, additional radial velocity data has been obtained using the 1.2m Euler telescope located at the La Silla observatory (see Groenewegen 2008A&amp;A...488...25G for a description of the data taking and data reduction). 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