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<ri:Resource created="2023-06-13T06:22:35Z" 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>(H-W2)-W1 vs W2-(BP-K) for 4 open cluster members</title><shortName>J/AJ/165/45</shortName><identifier>ivo://CDS.VizieR/J/AJ/165/45</identifier><altIdentifier>doi:10.26093/cds/vizier.51650045</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Malofeeva A.A.</name></creator><creator><name>Mikhnevich V.O.</name></creator><creator><name>Carraro G.</name></creator><creator><name>Seleznev A.F.</name></creator><date role="Updated">2023-10-17T11:43:38Z</date><date role="Created">2023-06-13T06:22:35Z</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>open-star-clusters</subject><subject>multiple-stars</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><description>In this study, we continue our project to search for unresolved binary and multiple systems in open clusters exploiting the photometric diagram (H-W2)-W1 versus W2-(BP-K) first introduced in Malofeeva+,. In particular, here we estimate the binary and multiple star ratios and the distribution of the component mass ratio q in the Galactic clusters AlphaPersei, Praesepe, and NGC1039. We have modified the procedure outlined in our first study making star counts automatic and by introducing bootstrapping for error estimation. Basing on this, we reinvestigated the Pleiades star cluster in the same mass range as in our previous work and corrected an inaccuracy in the mass ratio q distribution. The binary and multiple star ratio in the four clusters is then found to lie between 0.45{+/-}0.03 and 0.73{+/-}0.03. On the other hand, the ratio of systems with multiplicity more than 2 is between 0.06{+/-}0.01 and 0.09{+/-}0.02. The distribution of the component mass ratio q is well fitted with a Gaussian having the mode between 0.22{+/-}0.04 and 0.52{+/-}0.01 and the dispersion between 0.10{+/-}0.02 and 0.35{+/-}0.07. All clusters show a large number of the very low-mass secondary components in the binary systems with primary components below 0.5M{sun}.</description><source format="bibcode">2023AJ....165...45M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/165/45</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/VII/233">VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/123/1570">J/AJ/123/1570 : alpha Persei and Praesepe Clusters (Patience+, 2002)</relatedResource><relatedResource 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