J/A+A/675/A89ivo://CDS.VizieR/J/A+A/675/A89doi:10.26093/cds/vizier.36750089CDSDonada J.Anders F.Jordi C.Masana E.Gieles M.Perren G.I.,Balaguer-Nunez L.Castro-Ginard A.Cantat-Gaudin T.Casamiquela L.2024-11-28T20:04:29Z2023-07-04T08:54:22ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmilky-way-galaxyopen-star-clustersvisible-astronomyIn this study we provide a large homogeneous catalogue of multiplicity fractions in open clusters, including the unresolved and total (close- binary) multiplicity fractions of main-sequence systems with mass ratio larger than 0.6^+0.05^_-0.15_ for 202 open clusters in the extended solar neighbourhood (closer than 1.5kpc from the Sun). The unresolved multiplicity fractions are estimated applying a flexible mixture model to the observed Gaia colour-magnitude diagrams. Then we use custom Gaia simulations to account for the resolved systems and derive the total multiplicity fractions. The studied open clusters have ages between 6.6Myr and 3.0Gyr (146 are older than 50Myr and their member lists are taken from Tarricq et al. (2022A&A...659A..59T, Cat. J/A+A/659/A59), while the remaining 56 are younger than 50Myr and their member lists are taken from Cantat-Gaudin et al. (2020A&A...640A...1C, Cat. J/A+A/640/A1). Their total high-mass-ratio multiplicity fractions range between 6% and 80%, with a median of 18%. The multiplicity fractions increase with the mass of the primary star, as expected. The average multiplicity fraction per cluster displays an overall decreasing trend with the open cluster age up to ages about 100Myr, above which the trend increases. Our simulations show that most of this trend is caused by complex selection effects (introduced by the mass dependence of the multiplicity fraction and the magnitude limit of our sample). Furthermore, the multiplicity fraction is not significantly correlated with the clusters' position in the Galaxy. The spread in multiplicity fraction decreases significantly with the number of cluster members (used as a proxy for cluster mass). We also find that the multiplicity fraction decreases with metallicity, in line with recent studies using field stars.2023A&A...675A..89Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/675/A89CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)I/350 : Gaia EDR3 (Gaia Collaboration, 2020)J/A+A/640/A1 : Portrait Galactic disc (Cantat-Gaudin+, 2020)J/A+A/659/A59 : 389 local open clusters structural parameters (Tarricq+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/675/A89https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/675/A89http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/675/A89https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/675/A89https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/675/A89http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/675/A89GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/675/A89/catalog (Open cluster unresolved and total multiplicity fractions of main-sequence systems with mass ratio q>0.6^+0.05^_-0.15_)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/675/A89/catalog?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/675/A89/catalog?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/675/A89/catalog?GETtext/xml+votable180.050000true51.8734.9810.0055555555555555566/463 1297 1326 1347 1383 1386 1557 1576 1717 1913 2373 2381 2395 2463 2785 2859 2994 3201 3289 3308 3317 3556 6760 6869 6881 12891 13096 13874 13952 13962 13982 14033 14058 14094 14098 14103 14126 14162 14210 14233 14346 14373 14403 14410 14418 14553 14571 14603 14642 14732 14790 14878 15226 15396 15449 15622 15671 15686 15693 15747 16490 20797 20825 20853 21267 21325 21328 21450 21495 21522 21529 21531 21549 21562 21584 21656 21658 21774 21927 22018 22034 22058 22098 22123 22183 22805 22859 22880 22895 22993 23685 23769 24098 24291 24367 24399 28481 28800 28806-28807 28818 28997 29035 29101 29121 29158 29456 29728 29777 29865 29900 30114 30247 30439 30697 30717 31853 31865 32111 32122 33102 34538 37109 37224 37326 37594 37613 37679 37745 37789 37816-37817 37892 37945 38021 38051 38073 38119 38137 38562 38627 39003 39005 39018 39160 39172 39181 39191 39236 39244 39270 39285 39355 39369 39374-39375 39548 39739 39775 39785 39832 39867 39871 39894 40696 41314 41381 41436 41445 41461 41557-41558 41599 41675 41703 41788 41846 41995 42026 42029 42150 42203 42207 42268 42303 42376-42377 42503 42522 42850 43050 43136 43191 43218 43301 47621 47854 49099https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/675/A89?format=asciiOpticaldefaultJ/A+A/675/A89/catalogOpen cluster unresolved and total multiplicity fractions of main-sequence systems with mass ratio q>0.6^+0.05^_-0.15_fbtotqlim0.6Total multiplicity fraction (fb_tot_qlim0point6)stat.fit.paramfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintXX position in Galactic cartesian coordinates (X)pcpos.distance;pos.cartesian.x;pos.galacticfloat_RA.icrsRight ascension (ICRS) at Epoch=J2015.5 (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) at Epoch=J2015.5 (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedSimbadNameSimbad column added by the CDSmeta.idcharnullableRA_ICRSMean right ascension of members (ICRS) at Ep=2015.5 (RA_ICRS)degpos.eq.ra;meta.mainDE_ICRSMean declination of members (ICRS) at Ep=2015.5 (DE_ICRS)degpos.eq.dec;meta.mainGLONMean Galactic longitude of members (GLON)degpos.galactic.lonGLATMean Galactic latitude of members (GLAT)degpos.galactic.latfloatr50Radius containing half the members (r50)degphys.angSizefloatplxMean parallax of members (plx)maspos.parallax.trigfloate_plxStandard deviation of parallax of members (e_plx)masstat.error;pos.parallaxfloatlogAgeNNAge (logt) of the cluster (AgeNN)log(yr)time.agefloatAVNNExtinction Av of the cluster (AVNN)magphys.absorptionfloatDistPcDistance in parsecs (DistPc)pcpos.distancefloatYY position in Galactic cartesian coordinates (Y)pcpos.distance;pos.cartesian.y;pos.galacticfloatZZ position in Galactic cartesian coordinates (Z)pcpos.distance;pos.cartesian.z;pos.galacticfloatRgcDistance from Galactic centre assuming the Sun is at 8340pc (Rgc)pcpos.distancefloatnbMSmembNumber of selected main-sequence systems of the open cluster (nb_MS_members)meta.numberintBP-RP0minIntrinsic colour index BP-RP of the bluest selected system (BP_RP_0_min)magphot.color;em.opt.B;em.opt.VfloatBP-RP0maxIntrinsic colour index BP-RP of the reddest selected system (BP_RP_0_max)magphot.color;em.opt.B;em.opt.VfloatMSwidthBP-RP0max minus BP-RP0min (MS_width)magsrc.var.amplitudefloatMassMinMass interpolated for BP-RP0max using Parsec isochrone logage=7.2 (mass_min)solMassphys.massfloatMassMaxMass interpolated for BP-RP0min using Parsec isochrone logage=7.2 (mass_max)solMassphys.massfloatMassMeanMean mass of the open cluster's selected main-sequence members (mean_mass)solMassphys.massfloatfbqlim0.6Unresolved multiplicity fraction of systems having mass ratio larger than 0.6^+0.05^_-0.15_ (posterior pdf's 50th percentile) (fb_qlim0point6_50)stat.fit.paramfloatE_fbqlim0.6Unresolved multiplicity fraction posterior pdf's 84th percentile (fb_qlim0point6_sigu)stat.error;stat.maxfloate_fbqlim0.6Unresolved multiplicity fraction posterior pdf's 16th percentile (fb_qlim0point6_sigl)stat.errorfloatDGG magnitude offset between the polynomial functions fitted to the single and binary sequences (posterior pdf's 50th percentile) (DG_50)magphot.mag;arith.zpfloatE_DGDG_50 pdf's 84th percentile (DG_sigu)magstat.error;stat.maxfloate_DGDG_50 pdf's 16th percentile (DG_sigl)magstat.errorfloatsSStandard deviation in G magnitude of the single-sequence fitted Gaussian (posterior pdf's 50th percentile) (sS_50)magstat.stdev;phot.mag;meta.modelledfloatE_sSsS_50 pdf's 84th percentile (sS_sigu)magstat.error;stat.maxfloate_sSsS_50 pdf's 16th percentile (sS_sigl)magstat.errorfloatsBStandard deviation in G magnitude of the binary-sequence fitted Gaussian (posterior pdf's 50th percentile) (sB_50)magstat.stdev;phot.mag;meta.modelledfloatE_sBsB_50 pdf's 84th percentile (sB_sigu)magstat.error;stat.maxfloate_sBsB_50 pdf's 16th percentile (sB_sigl)magstat.errorfloatClusterOpen cluster name (Cluster)meta.id;meta.maincharE_fbtotqlim0.6Total multiplicity fraction 84th percentile (fb_tot_qlim0point6_sigu)stat.error;stat.maxfloate_fbtotqlim0.6Total multiplicity fraction 16th percentile (fb_tot_qlim0point6_sigl)stat.errorfloat