J/ApJ/828/46ivo://CDS.VizieR/J/ApJ/828/46doi:10.26093/cds/vizier.18280046CDSAnsdell M.Williams J.P.van der Marel N.Carpenter J.M.Guidi G.,Hogerheijde M.Mathews G.S.Manara C.F.Miotello A.Natta A.,Oliveira I.Tazzari M.Testi L.van Dishoeck E.F.van Terwisga S.E.2017-07-04T07:08:10Z2017-01-11T10:07:33ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsmillimeter-astronomysubmillimeter-astronomystellar-massesradio-astronomysurveysWe present the first high-resolution sub-millimeter survey of both dust and gas for a large population of protoplanetary disks. Characterizing fundamental properties of protoplanetary disks on a statistical level is critical to understanding how disks evolve into the diverse exoplanet population. We use the Atacama Large Millimeter/Submillimeter Array (ALMA) to survey 89 protoplanetary disks around stars with M*>0.1M_{sun}_ in the young (1-3Myr), nearby (150-200pc) Lupus complex. Our observations cover the 890{mu}m continuum and the ^13^CO and C^18^O 3-2 lines. We use the sub-millimeter continuum to constrain M_dust_ to a few Martian masses (0.2-0.4M_{Earth}_) and the CO isotopologue lines to constrain M_gas_ to roughly a Jupiter mass (assuming an interstellar medium (ISM)-like [CO]/[H_2_] abundance). Of 89 sources, we detect 62 in continuum, 36 in ^13^CO, and 11 in C^18^O at >3{sigma} significance. Stacking individually undetected sources limits their average dust mass to <~6 Lunar masses (0.03M_{Earth}_), indicating rapid evolution once disk clearing begins. We find a positive correlation between M_dust_ and M*, and present the first evidence for a positive correlation between M_gas_ and M*, which may explain the dependence of giant planet frequency on host star mass. The mean dust mass in Lupus is 3x higher than in Upper Sco, while the dust mass distributions in Lupus and Taurus are statistically indistinguishable. Most detected disks have M_gas_<~1M_Jup_ and gas-to-dust ratios <100, assuming an ISM-like [CO]/[H_2_] abundance; unless CO is very depleted, the inferred gas depletion indicates that planet formation is well underway by a few Myr and may explain the unexpected prevalence of super-Earths in the exoplanet population.2016ApJ...828...46Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/828/46CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/588/A108 : Spectra of CO and [CI] in protoplanetary disks (Kama+, 2016)J/A+A/561/A2 : 36 accreting YSOs emission lines (Alcala+, 2014)J/ApJ/749/79 : Transition disks. II. Southern MoC (Romero+, 2012)J/ApJ/724/835 : The Spitzer c2d survey of WTTSs. III. (Wahhaj+, 2010)J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)J/ApJS/177/551 : Spitzer c2d survey of Lupus dark clouds (Merin+, 2008)J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/828/46https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/828/46http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/828/46https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/828/46https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/828/46http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/828/46GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/828/46/table1 (*Stellar properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/828/46/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/828/46/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/828/46/table1?GETtext/xml+votable180.050000true234.8656917-34.77143610.005555555555555556Cone search capability for table J/ApJ/828/46/alma (The ALMA 890 micron continuum properties and gas data)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/828/46/alma?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/828/46/alma?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/828/46/alma?GETtext/xml+votable180.050000true234.865625-34.77154440.0055555555555555566/42595 42597 42598 42599 42605 42611 42614 42615 42704 42705 42713 42714 42727 42736 42737 427382.231961445672802e-22 2.231961445672802e-22https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/828/46?format=asciiRadiodefaultJ/ApJ/828/46/table1*Stellar propertiesSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource identifiermeta.id;meta.maincharprimaryAlink to ALMA datameta.ref.urlcharDist[150/200] Distancepcpos.distance;pos.heliocentricintSpTMK spectral typesrc.spTypecharMass[0.1/3]? Stellar masssolMassphys.massfloatnullablee_Mass[0.01/0.4]? Uncertainty MasssolMassstat.error;phys.massfloatnullableRef? Reference (1)meta.ref;pos.frameintnullable2MDisplay the 2MASS data (Cutri+ 2003, II/246) within 2"meta.ref.urlchar_RAPositions from SIMBAD (right ascension part)degpos.eq.ra;meta.main_DEPositions from SIMBAD (declination part)degpos.eq.dec;meta.mainJ/ApJ/828/46/almaThe ALMA 890 micron continuum properties and gas datal_F18COLimit flag on F18COmeta.code.errorcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource identifiermeta.id;meta.maincharRAJ2000[15/16] Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000[34/42] Degree of Declination (J2000)pos.eq.dec;meta.mainF890[-0.6/600] ALMA 890um continuum flux densitymJyphot.flux.density;em.mm.200-400GHzfloate_F890[0.1/90] Uncertainty in F890mJystat.errorfloatrms[0.2/0.7]? Root mean square; mJy/beammJy/beamstat.errorfloatnullablea[0.08/0.98]? Semi-major axisarcsecphys.angSize;srcfloatnullablee_a[0.001/0.03]? Uncertainty in aarcsecstat.errorfloatnullablePA[-86/59]? Position angledegpos.posAngintnullablee_PA[0/57]? Uncertainty in PAdegstat.errorintnullablei[0/82]? Inclinationdegsrc.orbital.inclinationintnullablee_i[0/28]? Uncertainty in idegstat.errorintnullableMDust[-0.24/141.1] Dust mass(5.97236x10+24kg)phys.massdoublee_MDust[0.04/21.2] Uncertainty in MDust(5.97236x10+24kg)stat.errorfloatl_F13COLimit flag on F13COmeta.code.errorcharF13CO[66/8880] Flux density of ^13^CO linemJy.km/sphot.flux.density;em.line.CO;spect.lineinte_F13CO[42/317]? Uncertainty in F13COmJy.km/sstat.errorintnullableF18CO[90/2410] Flux density of ^18^CO linemJy.km/sphot.flux.density;em.line.CO;spect.lineinte_F18CO[45/238]? Uncertainty in F18COmJy.km/sstat.errorintnullablel_MgasLimit flag on Mgasmeta.code.errorcharMgas[0.1/8.2] Gas mass(1.898187x10+27kg)phys.massfloatb_Mgas[0.3/3.1]? Lower boundary of Mgas(1.898187x10+27kg)phys.mass;stat.minfloatnullableB_Mgas[1/31.4]? Upper boundary of Mgas(1.898187x10+27kg)phys.mass;stat.maxfloatnullable