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<ri:Resource created="1998-08-31T13:19:02Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" 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/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>CCD photometry of SMC cluster Kron 3</title><shortName>J/AJ/112/2004</shortName><identifier>ivo://CDS.VizieR/J/AJ/112/2004</identifier><altIdentifier>doi:10.26093/cds/vizier.51122004</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Alcaino G.</name></creator><creator><name>Liller W.</name></creator><creator><name>Alvarado F.</name></creator><creator><name>Kravtsov V.</name></creator><creator><name>Ipatov A.,Samus N.</name></creator><creator><name>Smirnov O.</name></creator><date role="Updated">2023-04-06T16:50:22Z</date><date role="Created">1998-08-31T13:19:02Z</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>ccd-photometry</subject><subject>open-star-clusters</subject><description>We present BVRI CCD photometry of 3149 stars in the SMC populous cluster Kron 3. Radial dependence of the horizontal branch morphology has been revealed. Contrary to Rich et al. (1984ApJ...286..517R), we conclude that the cluster radius is about r=6'. We estimate the cluster metallicity as [Fe/H]=-1.26 and its apparent distance modulus as (m-M)=18.75mag. Our estimate of the cluster age, based on fitting isochrones of VandenBerg &amp; Bell (1985ApJS...58..561V) to our V-(B-V) and V-(V-R) diagrams, is about 10Gyr, the lower limit being 8Gyr; this values is greater than those derived earlier, presumably partially due to the distance modulus values used by earlier investigators being too large. Our age estimate is not far from the upper values from Righ et al. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Seq</name><description>Running number</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Xpos</name><description>x coordinate (along RA, increases to the east)</description><unit>pix</unit><ucd>pos.cartesian.x;instr.det</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Ypos</name><description>y coordinate (along DE, increases to the north)</description><unit>pix</unit><ucd>pos.cartesian.y;instr.det</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Vmag</name><description>V magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>B-V</name><description>B-V color index</description><unit>mag</unit><ucd>phot.color;em.opt.B;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>V-R</name><description>? 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