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<ri:Resource created="2026-05-28T12:15:34Z" status="active" updated="2026-05-28T14:29:54Z" 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>Contact binaries period-luminosity-metallicity</title><shortName>J/ApJ/961/248</shortName><identifier>ivo://CDS.VizieR/J/ApJ/961/248</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Song L.-Y.</name></creator><creator><name>Tian Z.-J.</name></creator><date role="Updated">2026-05-28T14:29:54Z</date><date role="Created">2026-05-28T12:15:34Z</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>spectroscopic-binary-stars</subject><subject>surveys</subject><subject>visible-astronomy</subject><subject>trigonometric-parallax</subject><subject>metallicity</subject><subject>ultraviolet-photometry</subject><subject>infrared-photometry</subject><description>Binary stars ubiquitous throughout the Universe are important. Contact binaries (CBs) possessing period-luminosity (PL) relations could be adopted as distance tracers. The PL relations of CBs are influenced by metallicity abundance and color index, which are connected to both the radius and luminosity of stars. Here we propose fine relations of the period-luminosity-metallicity-color (PLZC) from the ultraviolet to infrared bands based on current surveys. The accuracy of the distance estimation is 6% and 8%, respectively, depending on the PLZC relations of the CBs in the infrared and optical bands of the collected data. PLZC models are still more accurate than PLC models in determining intrinsic luminosity, notwithstanding their limited improvement. Meanwhile, these relations based on synthetic photometry are also calibrated. On the basis of the synthetic photometry, a 6% accuracy of distance is estimated. The measured or synthetic data of PLZC or PLC relations in infrared bands comes first in the list of suggestions for distance estimations and is followed by the measured data of optical bands.</description><source format="bibcode">2024ApJ...961..248S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/961/248</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/B/gcvs">B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/311">II/311 : WISE All-Sky Data Release (Cutri+ 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/328">II/328 : AllWISE Data Release (Cutri+ 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/335">II/335 : Revised catalog of GALEX UV sources (GUVcat_AIS GR6+7) (Bianchi+ 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/366">II/366 : ASAS-SN catalog of variable stars (Jayasinghe+, 2018-2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/355">I/355 : Gaia DR3 Part 1. 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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>Gaia</name><description>? 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GALEX FUV mean magnitude</description><unit>mag</unit><ucd>phot.mag;stat.mean;em.UV.100-200nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_FUVmag</name><description>[0.1/0.6]? Uncertainty in FUVmag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.UV.100-200nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>NUVmag</name><description>[14.96/22.93]? GALEX NUV mean magnitude</description><unit>mag</unit><ucd>phot.mag;stat.mean;em.UV.200-300nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_NUVmag</name><description>[0.007/0.5]? Uncertainty in NUVmag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.UV.200-300nm</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>GALEX</name><description>Display data from GALEX (II/335) within 3"</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>BPmag</name><description>[10.17/15.66]? Gaia DR3 BP mean magnitude</description><unit>mag</unit><ucd>phot.mag;stat.mean;em.opt.B</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_BPmag</name><description>[0.003/0.07]? Uncertainty in BPmag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.opt.B</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Gmag</name><description>[9.78/14.96]? 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WISE W1 mean magnitude</description><unit>mag</unit><ucd>phot.mag;em.IR.3-4um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W1mag</name><description>[0.02/0.04]? Uncertainty in W1mag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.IR.3-4um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W2mag</name><description>[8/12.7]? WISE W2 mean magnitude</description><unit>mag</unit><ucd>phot.mag;em.IR.4-8um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W2mag</name><description>[0.018/0.04]? Uncertainty in W2mag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.IR.4-8um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W3mag</name><description>[8.02/13.5]? WISE W3 mean magnitude</description><unit>mag</unit><ucd>phot.mag;stat.mean;em.IR.8-15um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W3mag</name><description>[0.016/0.6]? Uncertainty in W3mag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.IR.8-15um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>W4mag</name><description>[5.9/9.96]? WISE W4 mean magnitude</description><unit>mag</unit><ucd>phot.mag;stat.mean;em.IR.15-30um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W4mag</name><description>[0.07/0.6]? Uncertainty in W4mag</description><unit>mag</unit><ucd>stat.error;phot.mag;em.IR.15-30um</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>WISE</name><description>Display data from WISE (II/311) within 3"</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column></table></schema></tableset></ri:Resource>