J/ApJ/774/73ivo://CDS.VizieR/J/ApJ/774/73doi:10.26093/cds/vizier.17740073CDSIndebetouw R.Brogan C.Chen C.-H.R.Leroy A.Johnson K.Muller E.,Madden S.Cormier D.Galliano F.Hughes A.Hunter T.Kawamura A.,Kepley A.Lebouteiller V.Meixner M.Oliveira J.M.Onishi T.,Vasyunina T.2018-01-04T08:21:54Z2015-03-26T15:58:15ZCDS support team

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

cds-question@unistra.frmolecular-cloudsradio-astronomygalaxy-kinematicsmillimeter-astronomysubmillimeter-astronomyWe present Atacama Large (sub)Millimeter Array observations of 30 Doradus - the highest resolution view of molecular gas in an extragalactic star formation region to date (~0.4pcx0.6pc). The 30Dor-10 cloud north of R136 was mapped in ^12^CO 2-1, ^13^CO 2-1, C^18^O 2-1, 1.3mm continuum, the H30{alpha} recombination line, and two H_2_CO 3-2 transitions. Most ^12^CO emission is associated with small filaments and clumps (<~1pc, ~10^3^M_{sun}_ at the current resolution). Some clumps are associated with protostars, including "pillars of creation" photoablated by intense radiation from R136. Emission from molecular clouds is often analyzed by decomposition into approximately beam-sized clumps. Such clumps in 30 Doradus follow similar trends in size, linewidth, and surface density to Milky Way clumps. The 30 Doradus clumps have somewhat larger linewidths for a given size than predicted by Larson's scaling relation, consistent with pressure confinement. They extend to a higher surface density at a given size and linewidth compared to clouds studied at 10 pc resolution. These trends are also true of clumps in Galactic infrared-dark clouds; higher resolution observations of both environments are required. Consistency of clump masses calculated from dust continuum, CO, and the virial theorem reveals that the CO abundance in 30 Doradus clumps is not significantly different from the Large Magellanic Cloud mean, but the dust abundance may be reduced by ~2. There are no strong trends in clump properties with distance from R136; dense clumps are not strongly affected by the external radiation field, but there is a modest trend toward lower dense clump filling fraction deeper in the cloud.2013ApJ...774...73Ihttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/774/73CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/187 : 30 Doradus OB Associations (Parker 1992)J/ApJS/197/16 : CO observations of LMC molecular clouds (MAGMA). (Wong+, 2011)J/ApJS/196/18 : CO survey of galactic molecular clouds. II. (Bieging+, 2011)J/ApJS/191/160 : 3D spectroscopy in 30 Dor (Pellegrini+, 2010)J/ApJ/723/492 : GRS molecular clouds physical properties (Roman-Duval+, 2010)J/ApJS/184/172 : High- and intermediate-mass YSOs in the LMC (Gruendl+, 2009)J/ApJ/703/736 : Clump properties in the LMC 30 Dor region (Pineda+, 2009)J/ApJ/699/1092 : Giant molecular clouds (SRBY) (Heyer+, 2009)J/ApJ/686/948 : CO in extragalactic giant molecular clouds (Bolatto+, 2008)J/ApJS/178/56 : CO observations of LMC Giant Molecular clouds (Fukui+, 2008)J/AJ/136/18 : LMC SAGE. New candidate YSOs (Whitney+, 2008)J/A+A/471/103 : SIMBA observations of SMC (Bot+, 2007)J/ApJ/551/852 : FCRAO CO survey of the outer Galaxy (Heyer+, 2001)J/PASJ/53/971 : CO catalog of LMC molecular clouds (Mizuno+, 2001)J/A+A/341/98 : The ionizing cluster of 30 Doradus. I. (Selman+ 1999)J/A+AS/120/77 : Radio continuum study of the MC (Filipovic+, 1996)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/774/73https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/774/73http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/774/73https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/774/73https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/774/73http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/774/73GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/774/73/table3 (Clump properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/774/73/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/774/73/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/774/73/table3?GETtext/xml+votable180.050000true84.668875-69.08152780.0055555555555555566/33094https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/774/73?format=asciiRadiodefaultJ/ApJ/774/73/table3Clump propertiesSeq[1/103] Running sequence numbermeta.id;meta.mainintprimaryRAJ2000[5] Hour of right ascension (J2000)pos.eq.ra;meta.mainDEJ2000[69] Degree of declination (J2000)pos.eq.dec;meta.mainVel[234.5/264.5] CO velocitykm/sspect.dopplerVelocfloatRad[0.07/0.7] Radiuspcphys.size.radiusfloate_Rad[0.01/0.2] Rad uncertaintypcstat.errorfloatsigma[0.4/3.2] Velocity dispersion ({sigma}_v_)km/sphys.veloc.dispersionfloate_sigma[0/0.9] sigma uncertaintykm/sstat.errorfloat13COpk[0.6/24] ^13^CO(2-1) brightness temperatureKphys.temperaturefloatF13CO[0.2/86.1] ^13^CO(2-1) fluxK.km.s**-1.pc**2phot.fluxfloate_F13CO[0.1/2] F13CO uncertaintyK.km.s**-1.pc**2stat.errorfloat12COpk[2.1/62] ^12^CO(2-1) brightness temperatureKphys.temperaturefloatF12CO[0.5/410] ^12^CO(2-1) fluxK.km.s**-1.pc**2phot.fluxfloate_F12CO[0/0.8] F12CO uncertaintyK.km.s**-1.pc**2stat.errorfloatMmol[14/8528] Molecular masssolMassphys.massinte_Mmol[4/167] Mmol uncertaintysolMassstat.errorintMvir[21/4262] Virial masssolMassphys.massinte_Mvir[7/1816] Mvir uncertaintysolMassstat.errorintCommCommentmeta.noteSimbadSimbad column added by the CDSmeta.ref.urlchar