J/AJ/167/228ivo://CDS.VizieR/J/AJ/167/228doi:10.26093/cds/vizier.51670228CDSLuo A.-X.Liu H.-L.Qin S.-L.Yang D.-T.Pan S.2024-11-06T20:20:08Z2024-06-27T07:14:20ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsstar-forming-regionsinterstellar-mediumThis paper is aimed at exploring the implications of velocity-dispersion scalings on high-mass star formation in molecular clouds, including the scalings of Larson's linewidth-size ({sigma}-R) and ratio-mass surface density (L-{Sigma}; here L={sigma}/R0.5). We have systematically analyzed the {sigma} parameter of well-selected 221 massive clumps, complemented with published samples of other hierarchical density structures of molecular clouds over spatial scales of 0.01-10pc. Those massive clumps are classified into four phases: quiescent, protostellar, HII region, and PDR clumps in an evolutionary sequence. The velocity dispersion of clumps increases overall with the evolutionary sequence, reflecting enhanced stellar feedback in more evolved phases. The relations of {sigma}-R and L-{Sigma} are weak with the clump sample alone, but become evident when combined with others spanning a much wider spatial scales. For {sigma}-R, its tight relation indicates a kinematic connection between hierarchical density structures, supporting theoretical models of multiscale high-mass star formation. From the L-{Sigma} relation, cloud structures can be found to transition from overvirial state ({alpha}vir>2) to subvirial state ({alpha}vir<2) as they become smaller and denser, indicating a possible shift in the governing force from turbulence to gravity. This implies that the multiscale physical process of high-mass star formation hinges on the self-gravity of subvirial molecular clouds. However, the influence of turbulence may not be dismissed until large-scale clouds attain a subvirial state. This is pending confirmation from future multiscale kinematic observations of molecular clouds with uniform observing settings.2024AJ....167..228Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/167/228CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/481/345 : SED evolution in massive young stellar obj (Molinari+, 2008)J/ApJ/699/1092 : Giant molecular clouds (SRBY) (Heyer+, 2009)J/ApJ/723/492 : Physical property GRS molecular clouds (Roman-Duval+, 2010)J/MNRAS/443/1555 : ATLASGAL massive star forming clumps (Urquhart+, 2014)J/ApJ/815/130 : High-mass molecular clumps from MALT90 (Guzman+, 2015)J/A+A/575/A79 : SPIRE 250um maps of 4 molecular clouds (Schneider+, 2015)J/other/PASA/33.30 : MALT90 Catalogue (Rathborne+, 2016)J/MNRAS/477/2220 : Larson relations in massive clumps (Traficante+, 2018)J/MNRAS/473/1059 : Complete sample Galactic clump properties (Urquhart+, 2018)J/MNRAS/510/3389 : High-mass * formation evolutionary trends (Urquhart+, 2022)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/167/228https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/167/228http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/167/228https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/167/228https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/167/228http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/167/228GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/167/228/table1 (Physical properties of clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/167/228/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/167/228/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/167/228/table1?GETtext/xml+votable180.050000true272.36485-20.318690.0055555555555555565/7278 10542-10543 10624 6/29091 29094 29097 29099 29101 29103 29508 41595 41597 41655 41671 41673 41676-41677 41681 41683 41688 41759 41767 41770 41772 41776-41778 41780 41782 41799 41802 41804 41811-41813 41817 41820 41824-41825 42159 42207 42211 42213 42224 42226-42230 42376 42378-42379 42381-42383 42387 42390-42393 42396 42398 42434-42436 42438 42441 42501 42512 43013 43021 43024https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/167/228?format=asciidefaultJ/AJ/167/228/table1Physical properties of clumps_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexedrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintID[1/221] Clump sequential identifiermeta.id;meta.numberintSnameClump name, AGALDDD.ddd-DD.dddmeta.id;meta.maincharGLON[10.168/348.759] Galactic longitudedegpos.galactic.lonGLAT[-1.042/1.176] Galactic latitudedegpos.galactic.latRad[0.15/4.08] Clump radius (1)pcphys.size.radiusfloate_Rad[0.03/0.82] Uncertainty in Radius (1)pcstat.errorfloatSigma[0.04/0.42] average mass surface density (1)g.cm**-2phys.densityfloate_Sigma[0.0/0.05] Uncertainty in Sigma (1)g.cm**-2stat.errorfloatMass[27/64979] Clump masssolMassphys.massinte_Mass[10/19490] Uncertainty in MasssolMassstat.error;phys.massintLum[5/1040858]? Clump luminosity (2)solLumphys.luminosityintnullabledVel[0.23/3.2] Clump velocity dispersion at COkm.s**-1phys.veloc.dispersion;spect.linefloate_dVel[0.02/0.21] Uncertainty in dVkm.s**-1stat.errorfloatalpha[0.11/11.65] Virial parameterstat.fit.paramfloate_alpha[0.04/4.43] Uncertainty in alphastat.error;pos.eq.rafloatPhaseEvolutionary phasetime.phasechar