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<ri:Resource created="2001-08-12T18:25:11Z" 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>UBV light cures of KW Persei</title><shortName>J/A+A/373/950</shortName><identifier>ivo://CDS.VizieR/J/A+A/373/950</identifier><altIdentifier>doi:10.26093/cds/vizier.33730950</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Galis R.</name></creator><creator><name>Hric L.</name></creator><creator><name>Niarchos P.</name></creator><date role="Updated">2001-08-12T18:25:15Z</date><date role="Created">2001-08-12T18:25:11Z</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>eclipsing-binary-stars</subject><subject>visible-astronomy</subject><subject>broad-band-photometry</subject><description>The table 4 summarizes the photoelectric UBV magnitudes of the eclipsing binary KW Per. This observational material was taken at the Observatories of the Astronomical Institute of the Slovak Academy of Sciences at the Stara Lesna (SL) and Skalnate Pleso (SP), as well as at the Astronomical Station of the National Observatory of Athens at Kryonerion (KR). The observations were carried out in 25 runs (24 nights) during the period from December 4th 1996 to November 25th 1998 in 112 hours of pure observational time. At the observatories SL and SP identical Cassegrain telescopes with a diameter of 60 cm were used. The observations of KR were performed by the same type of telescope with diameter of the primary mirror 120 cm. An one-channel photoelectric photometer with digital converter was used, as well as standard UBV Johnson's filters. All observational data, collected in table 4 are in the form of phase and magnitude for U, B and V colours. 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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>Uphase</name><description>[0,1[? Phase in U colour</description><ucd>time.phase</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Umag</name><description>? KW Per U magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.U</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Bphase</name><description>[0,1[? Phase in B colour</description><ucd>time.phase</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Bmag</name><description>? KW Per B magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.B</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Vphase</name><description>[0,1[? Phase in V colour</description><ucd>time.phase</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Vmag</name><description>? KW Per V magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>