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<ri:Resource created="2024-09-24T10:17:24Z" status="active" updated="2026-07-03T06:36:09Z" 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>Multiplicity of stars with planets</title><shortName>J/A+A/689/A302</shortName><identifier>ivo://CDS.VizieR/J/A+A/689/A302</identifier><altIdentifier>doi:10.26093/cds/vizier/bc-nh/ldac</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Gonzalez-Payo J.</name></creator><creator><name>Caballero J.A.</name></creator><creator><name>Gorgas J.</name></creator><creator><name>Cortes-Contreras M.,Gelvez-Ortiz M.-C.</name></creator><creator><name>Cifuentes C.</name></creator><date role="Updated">2026-07-03T06:36:09Z</date><date role="Created">2024-09-24T10:17:24Z</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>multiple-stars</subject><subject>exoplanets</subject><subject>visible-astronomy</subject><subject>stellar-distance</subject><subject>proper-motions</subject><description>We intended to quantify the impact of stellar multiplicity on the presence and properties of exoplanets. We investigated all exoplanet host stars at less than 100 pc using the latest astrometric data from Gaia DR3 and advanced statistical methodologies. We complemented our search for common proper motion and parallax companions with data from the Washington Double Star catalogue and the literature. After excluding a number of systems based on radial velocity data, and membership in clusters and open associations, or with resolved ultracool companions, we kept 215 exoplanet host stars in 212 multiple-star systems. We found 17 new companions in the systems of 15 known exoplanet host stars, measured precise angular and projected physical separations and position angles for 236 pairs of stars, compiled key parameters for 276 planets in multiple systems, and established a comparison sample comprising 687 single stars with exoplanets. With all of this, we statistically analysed a series of hypothesis regarding planets in multiple stellar systems. Although they are only statistically significant at a 2{sigma} level, our analysis pointed to several interesting results on the comparison in the mean number of planets in multiple versus single stellar systems and the tendency of high mass planets to be located in closer orbits in multiple systems. We confirm that planets in multiple systems tend to have orbits with larger eccentricities than those in single systems. 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Distance</description><unit>pc</unit><ucd>pos.distance</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Dist</name><description>? Standard error of distance</description><unit>pc</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>l_rho</name><description>[~] Limit flag on rho</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>rho</name><description>? Projected physical separation between the current star and the first star of the system (not tabulated if rho &lt; 1 arcsec)</description><unit>arcsec</unit><ucd>pos.angDistance;src.orbital</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>theta</name><description>? Position angle of the current star relative to the first star of the system (not tabulated if rho &lt; 1 arcsec)</description><unit>deg</unit><ucd>pos.posAng</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Id</name><description>[1/212] System identification number</description><ucd>meta.id.parent</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>SimbadName</name><description>Simbad column added by the CDS</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="28*">char</dataType><flag>nullable</flag></column><column><name>Sep</name><description>? Separation</description><unit>au</unit><ucd>pos.distance;src.orbital</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>Ref</name><description>Literature reference(s)</description><ucd>meta.ref;pos.frame</ucd><dataType xsi:type="vs:VOTableType" arraysize="39*">char</dataType></column><column><name>WDS</name><description>Washington Double Star Id</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="10*">char</dataType></column><column><name>Host</name><description>[Yes/No ] It indicates whether the star hosts planets or not</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType" arraysize="3*">char</dataType></column></table></schema></tableset></ri:Resource>