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<ri:Resource created="2015-08-24T15:01:24Z" 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>V441 Lac VRI light curves</title><shortName>J/other/NewA/36.</shortName><identifier>ivo://CDS.VizieR/J/other/NewA/36.32</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wang D.</name></creator><creator><name>Zhang L.</name></creator><creator><name>Han X.L.</name></creator><creator><name>Agerer F.</name></creator><creator><name>Pi Q.</name></creator><creator><name>Wang S.</name></creator><date role="Updated">2017-06-26T11:49:16Z</date><date role="Created">2015-08-24T15:01:24Z</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>infrared-photometry</subject><subject>visible-astronomy</subject><subject>photometry</subject><description>We present the first multi-color VRI CCD light curves of a short-period eclipsing binary star v441 Lac in this paper. We obtained our light curves on Oct. 4 and 8, 2013 at Xinglong station of National Astronomical Observatories, China. We updated the ephemeris of V441 Lac based on three new minima derived by our new observational data together with previously available light curve minima. By fitting the O-C (observed minus calculated) values of the minima, we found that the orbital period of V441 Lac exhibits an increasing trend of View the dP/dt=5.67(0.35)x10^-7^days/year, which might be explained by mass transfer from the secondary component to the primary one, or angular momentum exchange by magnetic activities. We also obtained the photometric orbital parameters with the Wilson &amp; Devinney program. 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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>HJD</name><description>Heliocentric Julian Date of the minimum times</description><unit>d</unit><ucd>time.epoch</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>Cycle</name><description>[-1281/15397.5] Cycle</description><ucd>obs.proposal.cycle</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>(O-C)1</name><description>[-0.011/0.012] Residual of the linear fit</description><unit>d</unit><ucd>stat.fit.residual</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>(O-C)2</name><description>[-0.009/0.008] Residual of the polynomial fit</description><unit>d</unit><ucd>stat.fit.residual</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Source</name><description>[1/14] Reference (1)</description><ucd>meta.ref;pos.frame</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column></table><table><name>J/other/NewA/36.32/table2</name><description>The photometric data of V R I bands of V441 Lac</description><column><name>recno</name><description>Record number assigned by the VizieR team. 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