J/A+A/678/A20ivo://CDS.VizieR/J/A+A/678/A20doi:10.26093/cds/vizier.36780020CDSPrisegen M.Faltova N.2025-01-09T20:00:58Z2024-03-04T15:39:56ZCDS support team

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

cds-question@unistra.fropen-star-clusterswhite-dwarf-starsvisible-astronomystellar-massesstellar-agesOpen clusters (OCs) provide homogeneous samples of white dwarfs (WDs) with known distances, extinctions, and total ages. The unprecedented astrometric precision of Gaia allows us to identify many novel OC-WD pairs. Studying WDs in the context of their parent OCs makes it possible to determine the properties of WD progenitors and study the initial-final mass relation (IFMR). We seek to find potential new WD members of OCs in the solar vicinity. The analysis of OC members' parallaxes allows us to determine the OC distances to a high precision, which in turn enables us to calculate WD masses and cooling ages and to constrain the IFMR. We searched for new potential WD members of nearby OCs using the density-based machine learning clustering algorithm HDBSCAN. The clustering analysis was applied in five astrometric dimensions-positions in the sky, proper motions and parallaxes, and in three dimensions where the positional information was not considered in the clustering analysis. The identified candidate OC WDs were further filtered using the photometric criteria and properties of their putative host OCs. The masses and cooling ages of the WDs were calculated via a photometric method using all available Gaia, Pan-STARRS, SDSS, and GALEX photometry. The WD progenitor masses were determined using the ages and metallicities of their host OCs. Altogether, 63 OC WD candidates were recovered, 27 of which are already known in the literature. We provide characterization for 36 novel WDs that have significant OC membership probabilities. Six of them fall into relatively unconstrained sections of the IFMR where the relation seems to exhibit nonlinear behavior. We were not able to identify any WDs originating from massive progenitors that would even remotely approach the widely adopted WD progenitor mass limit of 8M_{sun}_; this confirms the paucity of such objects residing in OCs and hints at a presence of velocity kicks for nascent WDs.2023A&A...678A..20Phttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/678/A20CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/678/A20https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/678/A20http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/678/A20https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/678/A20https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/678/A20http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/678/A20GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/678/A20/table1 (WDs and WD candidates recovered as OC members in the clustering analysis)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/678/A20/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/678/A20/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/678/A20/table1?GETtext/xml+votable180.050000true286.283833336.95977780.0055555555555555566/2384 2433 2743 2784 3601 3603 3606 4685 4690 4696 4698-4699 4702 4709-4710 4720 4726 6049 14157 14644 14793 14914 15396 15424 15450 20459 20831 22132 23445 23618 28482 29045 29047 29118 29728 29730 30439 31812 31993 32111 32182 32188 33107 33126 37353 37583 37592-37593 37616 37926 37933 37942 37944 37946 38607 39350 41204 41834 42026 47278https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/678/A20?format=asciiOpticaldefaultJ/A+A/678/A20/table1WDs and WD candidates recovered as OC members in the clustering analysisSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintmoreindicates data in table2 and/or table3meta.ref.urlcharGaiaDR3Gaia DR3 source_idmeta.id;meta.mainprimaryAssocAssociated open clustermeta.id.parentcharP3D? Membership probability derived in the 3D membership analysisstat.probabilityfloatnullableP5D? Membership probability derived in the 5D membership analysisstat.probabilityfloatnullablePHR? Membership probability derived in the Hunt & Reffert (2023A&A...673A.114H, Cat. J/A+A/673/A114) membership analysisstat.probabilityfloatnullableFidAstrometric fidelity flag from Rybizki et al. (2022MNRAS.510.2597R)meta.code.memberfloatPWD? Probability of the object being a WD from Gentile Fusillo et al. (2021MNRAS.508.3877G, Cat. J/MNRAS/508/3877)stat.fit.goodnessfloatnullableDBM[Y] Y if the object is present as a spectroscopically confirmed WD in the Montreal White Dwarf Database (Dufour et al., 2017, ASP Conf. Ser., 509, 3, https://www.montrealwhitedwarfdatabase.org)meta.codechar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/A+A/678/A20/table2Literature WDs recovered as OC members in the clustering analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source_idmeta.id;meta.mainAssocAssociated open clustermeta.id.parentcharMWDWD masssolMassphys.massfloatE_MWDWD mass error (upper value)solMassstat.error;stat.maxfloate_MWDWD mass error (lower value)solMassstat.errorfloatMiProgenitor masssolMassphys.massfloatE_MiProgenitor mass error (upper value)solMassstat.error;stat.maxfloate_MiProgenitor mass error (lower value)solMassstat.errorfloatRefReference for WD and progenitor massesmeta.ref;pos.framecharJ/A+A/678/A20/table3Novel or previously uncharacterized WDs recovered as OC members in the clustering analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaDR3Gaia DR3 source_idmeta.id;meta.mainn_GaiaDR3[a-d] Note on GaiaDR3 (1)meta.notecharAssocAssociated open clustermeta.id.parentcharPmaxMaximum value of astrometric membership probability from P3D, P5D, and PHRstat.fit.goodnessfloatAPHOTAvailable photometrymeta.notecharMWDWD mass (2)solMassphys.massfloatE_MWDWD mass error (upper value)solMassstat.error;stat.maxfloate_MWDWD mass error (lower value)solMassstat.errorfloattcoolCooling age (2)Myrtime.ageintE_tcoolCooling age error (upper value)Myrstat.error;stat.maxinte_tcoolCooling age error (lower value)Myrstat.errorintMiProgenitor mass (2)solMassphys.massfloatE_MiProgenitor mass error (upper value)solMassstat.error;stat.maxfloate_MiProgenitor mass error (lower value)solMassstat.errorfloat