J/A+A/672/A29ivo://CDS.VizieR/J/A+A/672/A29doi:10.26093/cds/vizier.36720029CDSCordoni G.Milone A.P.Marino A.F.Vesperini E.Dondoglio E.,Vittoria Legnardi M.Mohandasan A.Carlos M.Lagioia E.P.Jang S.,Ziliotto T.2024-11-28T20:03:01Z2023-03-27T09:59:35ZCDS support team

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

cds-question@unistra.fropen-star-clustersmilky-way-galaxymultiple-starsgalaxy-classification-systemsBinary stars play a crucial role in the understanding of the formation and evolution of star clusters and their stellar populations. We use Gaia Data Release 3 to homogeneously analyze 78 Galactic open clusters and the unresolved binary systems composed of two main-sequence (MS) stars they host. We first investigated the clusters' structural parameters, such as the core radius and the central density and determined interpolating the density profile of each cluster, the cluster mass function (MF), and total mass. We measured the fraction of binaries with a large mass ratio and the fraction of blue straggler stars (BSSs), and, finally, we investigated possible connections between the populations of binary stars and BSSs with the main parameters of the host cluster. Remarkably, we find that the mass functions (MFs) of 78 analyzed open clusters follow a similar trend and are well reproduced by two single power-law functions, with a change in slope around masses of 1M_{sun}_. The fraction of binary stars ranges from ~15% to more than ~60% without significant correlation with the mass and the age of the host cluster. Moreover, we detect hints of a correlation between the total fraction of binary stars and the central density of the host cluster. We compared the fraction of binary stars with that of BSSs, finding that clusters with high and low central density exhibit different trends. The fraction of binaries does not significantly change with the mass of the primary star and the mass ratio. The radial distribution of binary stars depends on cluster age. The binaries of clusters younger than ~800Myr typically show a flat radial distribution, with some hints of a double peak. In contrast, the binaries of the remaining clusters are more centrally concentrated than the single stars, similar to what is observed in globular clusters.2023A&A...672A..29Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/672/A29CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/618/A93 : Gaia DR2 open clusters in the Milky Way (Cantat-Gaudin+ 2018)J/A+A/623/A108 : Age of 269 GDR2 open clusters (Bossini+, 2019)J/MNRAS/504/356 : Updated parameters of 1743 open clusters (Dias+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/672/A29https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/672/A29http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/672/A29https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/672/A29https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/672/A29http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/672/A29GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/672/A29/tablec1 (Cluster positions, proper motions, parameters and density profiles)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/672/A29/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/672/A29/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/672/A29/tablec1?GETtext/xml+votable180.050000true310.902823.89690.0055555555555555566/463 1302 1464 1930 3091 3796 4078 4298 4698 6149 6760 13096 13198 13952 14033 14162 14210 14575 14752 15121 20797 20833 20853 21529 21531 21538 21549 21557 21561 21656 21682 22021 24121 24291 24345 24522 29032 29081 29269 30215 30635 37351 37592 37705 37745 37789 37920 37933 39181 39216 39244 39374 39423 39775 39785 39867 39894-39895 39956 40071 40104 40451 40490 41445 41461 41599 41675 41688 41770 41834 42135 42164 42353 42420 43024 43036 43044https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/672/A29?format=asciiOpticaldefaultJ/A+A/672/A29/tablec1Cluster positions, proper motions, parameters and density profilesSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster identificationmeta.id;meta.maincharRAJ2000Right ascension (J2000.0) (1)degpos.eq.ra;meta.mainDEJ2000Right ascension (J2000.0) (1)degpos.eq.dec;meta.mainpmRAProper motion in RA (1)mas/yrpos.pm;pos.eq.rafloatpmDEProper motion in DE (1)mas/yrpos.pm;pos.eq.decfloatplxParallax (1)maspos.parallax.trigfloatDistDistance modulus (1)magphot.mag.distModfloatlogAgeLogarithm of Age (1)log(yr)time.agefloat[Fe/H]Metallicity (1)phys.abund.ZfloatAvExtiction Av of cluster (1)magphys.absorptionfloatNstarNumber of cluster membersmeta.numberintdr[0/1] Flag indicating if differential reddening correction appliedmeta.codeintrcCore radius in arcminarcminphys.angSize;srcdoublee_rcUncertainty in core radiusarcminstat.errordoublercpcCore radius in parsecpcphys.size.radiusdoublee_rcpcUncertainty in core radiuspcstat.errordoublemuCentral density in stars/arcmin^2^arcmin**-2src.densitydoublee_muUncertainty in central density in stars/arcmin^2^arcmin**-2stat.errordoublemupcCentral density in stars/parsec^2^pc**-2phys.densitydoublee_mupcUncertainty in central density in stars/parsec^2^pc**-2stat.errordoubleJ/A+A/672/A29/tablec2Mass functions, masses, binary and blue stragglers function for 78 open clusterse_fbss-MSError on blue stragglers fraction with respect to MS stars with 1mag below turn-offstat.errorfloatNbssNumber of blue straggler starsmeta.numberintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameCluster identificationmeta.id;meta.maincharmf-allMass function slope, all starsarith.grad;phys.massfloate_mf-allError mass function slope, all starsstat.errorfloatmf-lowMass function slope, low-mass starsarith.grad;phys.massfloate_mf-lowError mass function slope, low-mass starsstat.errorfloatmf-highMass function slope, high-mass starsarith.grad;phys.massfloate_mf-highError mass function slope, high-mass starsstat.errorfloatmass-singleCluster mass from single-slope mass functionphys.massdoubleRhalfmassHalf-mass radiusarcminphys.angSizedoubletrhHalf-mass relaxation time (1)Myrtime.relaxdoubleqlimMinimum mass ratio (qlim) considered to density binary starsphys.mass;arith.ratiofloatfbin-qlimBinary fraction with q>qlimphys.mass;arith.ratiofloate_fbin-qlimError on binary fraction with q>qlimstat.errorfloatfbin-totTotal extrapolated binary fraction with q>qlimphys.mass;arith.ratiofloate_fbin-totError total extrapolated binary fraction with q>qlimstat.errorfloatfbincore-totCore total binary fraction (only for clusters with Nstar>500)phys.mass;arith.ratiofloate_fbincore-totError core total binary fractionstat.errorfloatfbss-MSBlue stragglers fraction with respect to MS stars with 1mag below urn-offmeta.numberfloat