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<ri:Resource created="2009-02-10T13:40:06Z" status="active" updated="2025-09-29T20:17:40Z" 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>SDSS and Johnson-Cousins photometry of F-K stars</title><shortName>J/AN/329/790</shortName><identifier>ivo://CDS.VizieR/J/AN/329/790</identifier><altIdentifier>doi:10.26093/cds/vizier.113290790</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Just A.</name></creator><creator><name>Jahreiss H.</name></creator><date role="Updated">2025-09-29T20:17:40Z</date><date role="Created">2009-02-10T13:40:06Z</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>visible-astronomy</subject><subject>sloan-photometry</subject><subject>infrared-photometry</subject><subject>broad-band-photometry</subject><description>For an understanding of Galactic stellar populations in the SDSS filter system well defined stellar samples are needed. The nearby stars provide a complete stellar sample representative for the thin disc population. We compare the filter transformations of different authors applied to the main sequence stars from F to K dwarfs to SDSS filter system and discuss the properties of the main sequence. The location of the mean main sequence in colour-magnitude diagrams is very sensitive to systematic differences in the filter transformation. A comparison with fiducial sequences of star clusters observed in g', r', and i' show good agreement. 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