J/A+A/700/A235ivo://CDS.VizieR/J/A+A/700/A235CDSHsieh C.-H.Arce H.G.Maureira M.J.Pineda J.E.Segura-Cox D.,Mardones D.Dunham M.M.Li H.Offner S.S.R.2026-05-06T12:58:15Z2025-08-22T09:02:41ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsmillimeter-astronomysubmillimeter-astronomyeffective-temperatureThe 1.3mm CAMPOS survey has resolved 90 protostellar disks with ~15 au resolution across the Ophiuchus, Corona Australis, and Chamaeleon star-forming regions. To address the fundamental question, 'When does planet formation begins, we combined the CAMPOS sample with literature observations of Class 0-II disks (bolometric temperature, T_bol_<=1900K), all mapped at 1.3mm with resolutions ranging from 4 to 33au. To investigate substructure detection rates as a function of bolometric temperature, we restricted the sample to disks observed at the 1.3mm wavelength, with inclinations below 75 degrees, linear resolution <=20au and resolved with at least four resolution elements ({theta}_distk_/{theta}_res_?=4). We also considered the effects of extinction correction and the inclusion of Herschel Space Telescope data on the bolometric temperature measurements to constrain the lower and upper limits of bolometric temperature for each source. We find that by T_bol_~200-400K, substructure detection rates increased sharply to ~60%, corresponding to an approximate age of 0.2-0.4Myr. No substructures are detected in Class 0 disks. The ratio of disk-averaged brightness temperature to predicted dust temperature shows a trend of increasing values toward the youngest Class 0 disks, suggesting higher optical depths in these early stages. Our statistical analysis confirms that substructures similar to those in Class II disks are already common by the Class I stage, and the emergence of these structures at T_bol_~200-400K could represent only an upper limit. Classifying disks with substructures into those with and without large central cavities, we find both populations coexisting across evolutionary stages, suggesting they are not necessarily evolutionarily linked. If protostellar disk substructures do follow an evolutionary sequence, then our results imply that disk substructures evolve very rapidly and thus can be present in all Class I/II stages and/or that they can be triggered at different times.2025A&A...700A.235Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/700/A235CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/482/698 : Ophiuchus DIsc Survey Employing ALMA (ODISEA). I.J/ApJS/266/32 : Extension of HOPS out to 500pc (eHOPS). I. Aquilahttps://irsa.ipac.caltech.edu/data/Herschel/eHOPS/overview.html :https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/700/A235https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/700/A235http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/700/A235https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/700/A235https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/700/A235http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/700/A235GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/700/A235/tablea1 (Protostellar Disk substructure table)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/700/A235/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/700/A235/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/700/A235/tablea1?GETtext/xml+votable180.050000true246.6095833-24.40856110.0055555555555555566/1054 1082 1154 23549 29367 30741 30821 36956-36957 41132 42738 42959 42969-42970 42972 42981 42983 42989 42992 43010 47742 478281.528037907652962e-22 1.528037907652962e-22https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/700/A235?format=asciiMillimeterdefaultJ/A+A/700/A235/tablea1Protostellar Disk substructure tablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource Namemeta.id;meta.maincharprimarymoreMore in tables A2 and/or A3meta.ref.urlcharn_Name[+cef] Note on Name (1)meta.notecharClassProtostellar Classmeta.code.classcharn_Class[bd] Note on Class (1)meta.notecharTbolBolometric temperature from eHOPS survey (2)Kphys.temperatureintn_Tbol[a] Note on Tbol (1)meta.notecharTbolDBolometric temperature from Dunham et al., 2015ApJS..220...11D, Cat. J/ApJS/220/11 (3)Kphys.temperatureintLbolBolometric luminositysolLumphys.luminosityfloatMassDisk dust mass1e-05solMassphys.massfloatR90Radius of the disk containing 90% of fluxauphys.angSize;srcfloatDistDistance to the sourcepcpos.distanceintSimbadNameSimbad column added by the CDSmeta.idcharnullable_RAPositions from Simbad and reference lists (right ascension part)degpos.eq.ra;meta.main_DEPositions from Simbad and reference lists (declination part)degpos.eq.dec;meta.mainF1.3mmTotal disk continuum flux at 1.3mm (ALMA Band 6)mJyphot.flux.density;em.IR.JfloatTypeType of substructure (4)meta.code.classcharBeam1Beam sizemasphys.angSize;instr.beamintBeam2Beam sizemasphys.angSize;instr.beamintResLinear Resolution of the observationaupos.distance;pos.angResolution;obsfloatTbrPBrightness temperature from full Planck equationKphys.temperaturefloatTdustDust temperature of the disk adopting equationKphys.temperaturefloatRefReferences (For RA, Dec see references) (5)meta.refcharCloudMolecular Cloud identifiermeta.id.parentcharJ/A+A/700/A235/tablea2Cross matching Corona Australis, Chamaeleon I & II, Ophiuchus North, and Ophiuchus sources in our CAMPOS surveyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the sourcemeta.id;meta.maincharCAMPOSCAMPOS ID (1)meta.idcharSSTgbs/SSTc2dSSTgbs/SSTc2d Names (2)meta.idchareHOPSeHOPS Name (3)meta.idcharISOInfrared Space Observatory Name (4)meta.idcharIRASInfrared Astronomical Satellite Name (5)meta.idcharCloudMolecular Cloud identifiermeta.id.parentcharJ/A+A/700/A235/tablea3Cross Matching ODISEA Survey with eHOPS and SSTgbs/SSTc2drecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintODISEAODISEA source ID, ODISEA C4 NNNmeta.id;meta.maincharSSTgbs/SSTc2dSSTgbs/SSTc2d Namesmeta.idcharNameeHOPS Name (1)meta.idcharOtherOther Name (2)meta.idcharIncluded?[Y/N] Included in the paper (Yes/No)meta.codecharNoteOther Notesmeta.notechar