J/ApJ/874/16ivo://CDS.VizieR/J/ApJ/874/16doi:10.26093/cds/vizier.18740016CDSLiu M.Tan J.C.De Buizer J.M.Zhang Y.Beltran M.T.Staff J.E.,Tanaka K.E.I.Whitney B.Rosero V.2021-01-05T10:53:32Z2020-09-14T08:05:20ZCDS support team

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

cds-question@unistra.frinfrared-photometryinterstellar-mediumstar-forming-regionsWe present multiwavelength images observed with SOFIA-FORCAST from ~10 to 40{mu}m of seven high luminosity massive protostars, as part of the SOFIA Massive Star Formation Survey. Source morphologies at these wavelengths appear to be influenced by outflow cavities and extinction from dense gas surrounding the protostars. Using these images, we build spectral energy distributions (SEDs) of the protostars, also including archival data from Spitzer, Herschel, and other facilities. Radiative transfer (RT) models of Zhang & Tan (2018ApJ...853...18Z), based on Turbulent Core Accretion theory, are then fit to the SEDs to estimate key properties of the protostars. Considering the best five models fit to each source, the protostars have masses m*~12-64M_{sun}_ accreting at rates of dm/dt_*_~10^-4^-10^-3^M_{sun}_/yr inside cores of initial masses M_c_~100-500M_{sun}_ embedded in clumps with mass surface densities {Sigma}_cl_~0.1-3g/cm^2^ and span a luminosity range of 10^4^-10^6^L_{sun}_. Compared with the first eight protostars in Paper I (De Buizer+ 2017ApJ...843...33D), the sources analyzed here are more luminous and, thus, likely to be more massive protostars. They are often in a clustered environment or have a companion protostar relatively nearby. From the range of parameter space of the models, we do not see any evidence that {Sigma}cl needs to be high to form these massive stars. For most sources, the RT models provide reasonable fits to the SEDs, though the cold clump material often influences the long wavelength fitting. However, for sources in very clustered environments, the model SEDs may not be such a good description of the data, indicating potential limitations of the models for these regions.2019ApJ...874...16Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/874/16CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/319 : UKIDSS-DR9 LAS, GCS and DXS Surveys (Lawrence+ 2012)II/328 : AllWISE Data Release (Cutri+ 2013)J/ApJS/91/659 : Ultracompact HII regions radio images (Kurtz+ 1994)J/MNRAS/291/261 : Methanol maser of IRAS-selected sources (Walsh+ 1997)J/MNRAS/301/640 : Ultracompact H II regions studies. II. (Walsh+, 1998)J/ApJ/587/714 : H_2_CO and H{alpha} observations of UC HII (Watson+, 2003)J/ApJ/702/1615 : CH_3_OH maser survey of EGOs (Cyganowski+, 2009)J/ApJ/707/89 : Variation of mid-IR extinction (Gao+, 2009)J/A+A/510/A89 : RMS survey of young massive stars in far-IR (Mottram+, 2010)J/A+A/525/A149 : Red MSX Survey (RMS): YSO bolometric fluxes (Mottram+, 2011)J/A+A/534/A131 : Clumps in the giant molecular cloud G345.5+1.0 (Lopez+, 2011)J/A+A/558/A24 : The VLTI/MIDI survey of Massive YSOs (Boley+, 2013)J/A+A/593/A49 : G35.20-0.74N VLA continuum images (Beltran+, 2016)J/A+A/595/A88 : G345.45+1.50 ^13^CO(3-2) clumps (Lopez-Calderon+, 2016)J/ApJ/843/33 : SOMA Star Formation Survey. Paper I. (De Buizer+, 2017)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/874/16https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/874/16http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/874/16https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/874/16https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/874/16http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/874/16GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/874/16/table1 (SOFIA-FORCAST observations: observation dates and exposure times)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/874/16/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/874/16/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/874/16/table1?GETtext/xml+votable180.050000true288.3660791710.89351250.0055555555555555566/30319 30644 30694 41655 41677 42207 42398https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/874/16?format=asciiInfrareddefaultJ/ApJ/874/16/table1SOFIA-FORCAST observations: observation dates and exposure timesSimbadNameSimbad column added by the CDSmeta.idcharNameName of the protostarmeta.id;meta.maincharprimaryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Hour of right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Degree of declination (J2000)pos.eq.dec;meta.mainDist[1.7/10.2] Distancekpcpos.distance;pos.heliocentricfloatRap[16/48] Aperture radius in arcsecarcsecphys.angSize;srcintRap_pc[0.26/1.72] Aperture radius in pcpcphys.size.radiusfloatDateUT date of observationtime.epoch;obsnullableExp7.7[290/2443] 7.7um exposure timestime.duration;obs.exposure;em.IR.4-8umintExp19.7[716/882] 19.7um exposure timestime.duration;obs.exposure;em.IR.15-30umintExp31.5[502/664] 31.5um exposure timestime.duration;obs.exposure;em.IR.30-60umintExp37.1[1028/1691] 37.1um exposure timestime.duration;obs.exposure;em.IR.30-60umintNfNumber of integrated flux density measurementsmeta.numberintnullableFitDisplay the parameters of the best five fitted models (link to Table 4)meta.ref.urlcharSEDIR fluxes interactive plotmeta.ref.urlcharJ/ApJ/874/16/fluxesIntegrated flux densities (from Table 2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource identifiermeta.id;meta.maincharTelFacilitymeta.notecharlambda[3.4/500] Wavelengthumem.wlfloatFfix[0.1/5848]? Fixed aperture flux density with background subtractionJyphot.flux.density;em.IRfloatnullableFfixpre[0.3/6205]? Fixed aperture flux density without background subtractionJyphot.flux.density;em.IRfloatnullableFvar[0.05/5848]? Variable aperture flux density with background subtractionJyphot.flux.density;em.IRfloatnullableFvarpre[0.07/6205]? Variable aperture flux density without background subtractionJyphot.flux.density;em.IRfloatnullableRap[2/48]? Aperture radiusarcsecphys.angSize;srcfloatnullableJ/ApJ/874/16/table4Parameters of the best five fitted modelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource identifiermeta.id;meta.maincharchi2[0.53/69.3] Model {chi}^2^/degrees of freedomstat.fit.dof;stat.param;meta.modelledfloatMc[80/480] Initial core masssolMassphys.massintSigma[0.1/3.2] Clump mean mass surface densityg.cm**-2phys.density;stat.meanfloatRc-Phy[0.03/0.51] Physical initial core radiuspcphys.size.radiusfloatRc-Ang[1/62] Angular initial core radiusarcsecphys.angSizeintM*[12/64] Current protostellar masssolMassphys.massfloattheta[13/71] Viewing angledeginstr.offsetintAv[0/100] Foreground extinction in the V bandmagphys.absorptionfloatMenv[35/459] Current envelope masssolMassphys.massinttheta-esc[10/45] Half opening angle of outflow cavitydeginstr.offsetintdM/dt[0.00014/0.002] Disk accretion rate to starsolMass/yrphys.mass.lossfloatLiso[33000/1300000] Bolometric luminosity assuming isotropic radiationsolLumphys.luminosityfloatLbol[40000/840000] True bolometric luminosity, inclination correctedsolLumphys.luminosityfloat