J/A+A/695/A257ivo://CDS.VizieR/J/A+A/695/A257doi:10.26093/cds/vizier/bc-nq/lcfhCDSRicciardi G.Van Terwisga S.E.Roccatagliata V.Hacar A.Henning T.,Del Pozzo W.2026-07-03T06:36:41Z2025-08-28T08:55:36ZCDS support team

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

cds-question@unistra.frmolecular-cloudsmultiple-starsstellar-massesObservations of protoplanetary disks within multiple systems in nearby star-forming regions (SFRs) have shown that the presence of a neighboring object influences the evolution of dust in disks. However, the size of the available sample and the separation range covered are insufficient to fully understand the dust evolution in binary systems. The goal of this work, based on the Survey of Orion Disks with ALMA (SODA), is to comprehensively characterize the impact of stellar multiplicity on Class II disks in the L1641 and L1647 regions of Orion A (~1-3Myr). We characterized the protostellar multiplicity using the Atacama Large Millimeter/submillimeter Array (ALMA), the ESO-VISTA, and the Hubble Space Telescope. The resulting sample of 65 multiple systems is the largest catalog of wide binary systems to date (projected separation >=1000AU) and enables a more robust statistical characterization of the evolution and properties of protoplanetary disks. The disk population was observed in the continuum with ALMA at 225GHz, with a median rms of 1.5M_{Earth}_. We combined these data (resolution of ~1.1") with the ESO-VISTA near-infrared survey of the Orion A cloud (resolution of ~0.7"). From this dataset, multiple-star systems were selected using an iterative inside-out search in projected separation (>=1000AU). We identify 61 binary systems, 3 triple systems, and 1 quadruple system. The separation range is between 1000 and 104AU. The dust mass distributions inferred via the Kaplan-Meier estimator yield a median mass of 3.23_-0.4_^+0.6^M_{Earth}_ for primary disks and 3.88_-0.3+_^0.3^M_{Earth}_ for secondary disks. Combining our data with those available for the Lupus and Taurus disks, we identify a threshold separation of about 130AU, beyond which the previously observed positive correlation between millimeter flux (and hence dust mass) and projected separation is lost. Recent theoretical models confirm that pre- and post-threshold systems are the result of different star formation processes, such as the fragmentation of gravitationally unstable circumstellar disks, the thermal fragmentation of infalling cores, or the turbulent fragmentation of molecular clouds. We can rule out the dependence on different SFRs: the cumulative mass distributions of multiples in SFRs of similar ages are statistically indistinguishable. This result strengthens the hypothesis that there is a universal initial mass distribution for disks.2025A&A...695A.257Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/695/A257CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/AJ/144/192 : Spitzer survey of Orion A and B. I. YSO catalogJ/ApJ/818/59 : IN-SYNC. IV. YSOs in Orion A (Da Rio+, 2016)J/ApJ/821/52 : NIR survey of Spitzer YSOs in Orion Mol. CloudJ/A+A/622/A149 : Vienna survey in Orion. III. (Grossschedl+, 2019)J/A+A/661/A53 : Survey of Orion disks with ALMA (SODA) (van Terwisga+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/695/A257https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/695/A257http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/695/A257https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/695/A257https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/695/A257http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/695/A257GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/695/A257/tabled1 (Multiple systems in the L1641 and L1647 regions of Orion A)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/695/A257/tabled1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/695/A257/tabled1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/695/A257/tabled1?GETtext/xml+votable180.050000true84.0277319-6.24054640.0055555555555555566/21438-21439 22805 22848 22854-22855https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/695/A257?format=asciidefaultJ/A+A/695/A257/tabled1Multiple systems in the L1641 and L1647 regions of Orion ArecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMassesDSindicates disk dust and stellar masses in table d2meta.ref.urlcharSystemBinary of the multiple system (Vision Index) (ID1-ID2) (1)meta.id;meta.maincharprimaryn_System[b] b when same ID1 and ID2meta.notecharSystem3? Third of the multiple system (Vision Index)meta.id.part;meta.mainintnullableSystem4? Forth of the multiple system (Vision Index)meta.id.part;meta.mainintnullableSepSeparationaupos.distance;src.orbitalfloatMassMean masssolMassphys.mass;stat.meanfloate_MassMean mass errorsolMassstat.error;phys.massfloatDistAverage Distancepcpos.distanceintSimbadSimbad column added by the CDSmeta.ref.urlchar_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/695/A257/tabled2Stellar massesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSystemBinary of the multiple system (VISION Index)meta.id;meta.maincharMassDD1Disk dust mass 1st source (1)solMassphys.massfloate_MassDD1Disk dust mass 1st source errorsolMassstat.errorfloatMassDD2Disk dust mass 2nd source (1)solMassphys.massfloate_MassDD2Disk dust mass 2nd source errorsolMassstat.errorfloatMassS1? Stellar mass 1st source (2)solMassphys.massfloatnullablee_MassS1? Stellar mass 1st source errorsolMassstat.errorfloatnullableMassS2? Stellar mass 2nd source (2)solMassphys.massfloatnullablee_MassS2? Stellar mass 2nd source errorsolMassstat.errorfloatnullable