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<ri:Resource created="2013-09-16T12:56:19Z" 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>CCD CT1 data of stars in the field of B119</title><shortName>J/MNRAS/425/3085</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/425/3085</identifier><altIdentifier>doi:10.26093/cds/vizier.74253085</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Piatti A.E.</name></creator><creator><name>Bica E.</name></creator><date role="Updated">2024-07-18T20:19:11Z</date><date role="Created">2013-09-16T12:56:19Z</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>magellanic-clouds</subject><subject>stellar-associations</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><description>We present for the first time Washington CT_1_ photometry for 11 unstudied or poorly studied candidate star clusters. The selected objects are of small angular size, contain a handful of stars, and are projected towards the innermost regions of the Small Magellanic Cloud (SMC). The respective colour-magnitude diagrams (CMDs) were cleaned of the unavoidable star field contamination by taking advantage of a procedure which makes use of variable size CMD cells. This method has shown to be able to eliminate stochastic effects in the cluster CMDs caused by the presence of isolated bright stars, as well as to make a finer cleaning in the most populous CMD regions. 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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>Star sequential number</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Xpos</name><description>X position (1)</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 position (1)</description><unit>pix</unit><ucd>pos.cartesian.y;instr.det</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>T1mag</name><description>T1 magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.R</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_T1mag</name><description>rms uncertainty on T1mag</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>C-T1</name><description>C-T1 colour index</description><unit>mag</unit><ucd>phot.color;em.opt.U;em.opt.R</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_C-T1</name><description>rms uncertainty on C-T1</description><unit>mag</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>_RA</name><description>Position computed from a comparison with IRSF catalog I/288 ({sigma}=0.1'') (right ascension part)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Position computed from a comparison with IRSF catalog I/288 ({sigma}=0.1'') (declination part)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table></schema></tableset></ri:Resource>