J/A+A/671/A1ivo://CDS.VizieR/J/A+A/671/A1doi:10.26093/cds/vizier.36710001CDSOlivares J.Bouy H.Miret-Roig N.Galli P.A.B.Sarro L.M.Moraux E.,Berihuete A.2024-11-06T20:02:53Z2023-02-28T16:07:02ZCDS support team

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

cds-question@unistra.fropen-star-clustersextinctionvisible-astronomystellar-massesStar-forming regions are excellent benchmarks for testing and validating theories of star formation and stellar evolution. The Perseus star-forming region, being one of the youngest (<10Myr), closest (280-320pc), and most studied in the literature, is a fundamental benchmark. We aim to study the membership, phase-space structure, mass, and energy (kinetic plus potential) distribution of the Perseus star-forming region using public catalogues (Gaia, APOGEE, 2MASS, and Pan-STARRS). We used Bayesian methodologies that account for extinction to identify the Perseus physical groups in the phase-space, retrieve their candidate members, derive their properties (age, mass, 3D positions, 3D velocities, and energy), and attempt to reconstruct their origin. Results. We identify 1052 candidate members in seven physical groups (one of them new) with ages between 3 and 10Myr, dynamical super-virial states, and large fractions of energetically unbounded stars. Their mass distributions are broadly compatible with that of Chabrier for masses >~0.1M_{sun}_ and do not show hints of over-abundance of low-mass stars in NGC1333 with respect to IC348. These groups' ages, spatial structure, and kinematics are compatible with at least three generations of stars. Future work is still needed to clarify if the formation of the youngest was triggered by the oldest. The exquisite Gaia data complemented with public archives and mined with comprehensive Bayesian methodologies allow us to identify 31% more members than previous studies, discover a new physical group (Gorgophone: 7Myr, 191 members, and 145M_{sun}_), and confirm that the spatial, kinematic, and energy distributions of these groups support the hierarchical star formation scenario.2023A&A...671A...1Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A1CatalogResearchIsServedByTAP 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/671/A1https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/671/A1http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/671/A1https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/671/A1https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/671/A1http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/671/A1GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/671/A1/tablec1 (Properties of the 1052 candidate members)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/671/A1/tablec1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/671/A1/tablec1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/671/A1/tablec1?GETtext/xml+votable180.050000true56.050546697891830.1477469679340.0055555555555555565/215 384-386 6/853-855 857 859 881 884-885 1193-1196 1198-1199 1548https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/671/A1?format=asciiOpticaldefaultJ/A+A/671/A1/tablec1Properties of the 1052 candidate members_RA.icrsRight ascension (ICRS) at Epoch=J2016. (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=J2016. (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.decindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGroupParent statistical group (statistical_group) (1)meta.id.parentcharGaiaDR3? Gaia DR3 source_id (source_id)meta.id;meta.mainnullableRA_ICRS[51.23/59.0] Right ascension (ICRS) at Ep=2016.0 (from Gaia DR3) (ra)degpos.eq.ra;meta.mainDE_ICRS[30.0/33.0] Declination (ICRS) at Ep=2016.0 (from Gaia DR3) (dec)degpos.eq.dec;meta.mainmeanX[111.98/202.89] Mean value of the Cartesian X position (mean_X)pcpos.distance;pos.cartesian.x;stat.meanfloate_meanX[0.49/10.95] Standard deviation of the Cartesian X position (sd_X)pcstat.errorfloatmeanY[174.0/307.1] Mean value of the Cartesian Y position (mean_Y)pcpos.distance;pos.cartesian.y;stat.meanfloate_meanY[0.72/16.32] Standard deviation of the Cartesian Y position (sd_Y)pcstat.errorfloatmeanZ[125.39/217.24] Mean value of the Cartesian Z position (mean_Z)pcpos.distance;pos.cartesian.z;stat.meanfloate_meanZ[0.55/11.22] Standard deviation of the Cartesian Z position (sd_Z)pcstat.errorfloatmeanU[-1.28/9.53] Mean value of the Cartesian U velocity (mean_U)km/sphys.veloc;pos.cartesian.xfloate_meanU[0.05/1.65] Standard deviation of the Cartesian U velocity (sd_U)km/sstat.errorfloatmeanV[15.47/25.3] Mean value of the Cartesian V velocity (mean_V)km/sphys.veloc;pos.cartesian.yfloate_meanV[0.05/2.25] Standard deviation of the Cartesian V velocity (sd_V)km/sstat.errorfloatmeanW[-8.04/4.66] Mean value of the Cartesian W velocity (mean_W)km/sphys.veloc;pos.cartesian.zfloate_meanW[0.05/1.63] Standard deviation of the Cartesian W velocity (sd_W)km/sstat.errorfloatb_mapmass[0.02/17.55] Percentile 2.5 of the system mass (lower_mass)solMassphys.massdoublemapmass[0.02/17.87] Maximum-a-posteriori of the system mass (map_mass)solMassphys.massdoubleB_mapmass[0.03/17.96] Percentile 97.5 of the system mass (upper_mass)solMassphys.massdoubleb_mapAv[0.03/9.12] Percentile 2.5 of the Av extinction (lower_Av)magphys.absorptiondoublemapAv[0.0/9.99] Maximum-a-posteriori of the Av extinction (map_Av)magphys.absorptiondoubleB_mapAv[0.31/9.9] Percentile 97.5 of the Av extinction (upper_Av)magphys.absorptiondouble