J/A+A/637/A40ivo://CDS.VizieR/J/A+A/637/A40doi:10.26093/cds/vizier.36370040CDSZhang S.Zavagno A.Yuan J.Liu H.Figueira M.Russeil D.,Schuller F.Marsh K.A.Wu Y.2021-12-07T10:47:33Z2020-05-12T08:46:06ZCDS support team

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

cds-question@unistra.frh-ii-regionsmillimeter-astronomysubmillimeter-astronomystellar-associationsinterstellar-mediumThe role of ionization feedback on high-mass (>8M_{sun}_) star formation is still highly debated. Questions remain concerning the presence of nearby HII regions changes the properties of early high-mass star formation and whether H ii regions promote or inhibit the formation of high-mass stars. To characterize the role of HII regions on the formation of high-mass stars, we study the properties of a sample of candidates high-mass starless clumps (HMSCs), of which about 90% have masses larger than 100 Msun. These high-mass objects probably represent the earliest stages of high-mass star formation; we search if (and how) their properties are modified by the presence of an HII region. We took advantage of the recently published catalog of HMSC candidates. By cross matching the HMSCs and HII regions, we classified HMSCs into three categories: 1) The HMSCs associated with HII regions both in the position in the projected plane of the sky and in velocity; 2) HMSCs associated in the plane of the sky, but not in velocity; and 3) HMSCs far away from any HII regions in the projected sky plane. We carried out comparisons between associated and non-associated HMSCs based on statistical analyses of multiwavelength data from infrared to radio. We show that there are systematic differences of the properties of HMSCs in different environments. Statistical analyses suggest that HMSCs associated with HII regions are warmer, more luminous, more centrally-peaked and turbulent. We also clearly show, for the first time, that the ratio of bolometric luminosity to envelope mass of HMSCs (L/M) could not be a reliable evolutionary probe for early massive star formation due to the external heating effects of the HII regions. We show HMSCs associated with HII regions present statistically significant differences from HMSCs far away from HII regions, especially for dust temperature and L/M. More centrally peaked and turbulent properties of HMSCs associated with HII regions may promote the formation of high-mass stars by limiting fragmentation. High-resolution interferometric surveys toward HMSCs are crucial to reveal how HII regions impact the star formation process inside HMSCs.2020A&A...637A..40Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/637/A40CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJS/231/11 : ATLASGAL high-mass starless clump candidates (Yuan+, 2017)J/MNRAS/473/1059 : Complete sample of Galactic clump propertieshttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/637/A40https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/637/A40http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/637/A40https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/637/A40https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/637/A40http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/637/A40GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/637/A40/table4 (Basic properties of high-mass starless clump candidates)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/637/A40/table4?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/637/A40/table4?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/637/A40/table4?GETtext/xml+votable180.050000true266.2252917-28.80061110.0055555555555555565/10556 10614 6/28808-28809 28814 28824-28825 28827-28828 28830-28831 28874-28875 28879 28890 28897 28900-28901 28912-28913 28915 28918-28919 29090-29091 29097 29099 29101 29103 29113 29115-29116 29118-29119 29463 29505 29508 29510 29529 29532-29533 29535 30218 30241 30244-30245 30256 30259-30260 30262 30268-30269 30312-30313 30315 30319 30618 30644 30694 41655 41767 41780 41782 41811-41814 41817 41820 42159 42169 42171-42173 42175 42206-42207 42214-42215 42217 42228 42378-42379 42387 42391 42396 42441 42444 42447 42460-42462 42496-42498https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/637/A40?format=asciiMillimeterdefaultJ/A+A/637/A40/table4Basic properties of high-mass starless clump candidatesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of sources, GLLL.llll+B.bbbmeta.id;meta.maincharTdustDust temperature (1)Kphys.temperaturefloatnH2Molecular hydrogen number densitycm**-3meta.number;phys.densitydoublee_nH2Error of molecular hydrogen number densitycm**-3stat.errordoubleNH2Molecular hydrogen column densitycm**-2phys.columnDensitydoublee_NH2Error of molecular hydrogen column density (2)cm**-2stat.error;phys.columnDensitydoubleMclumpMass of clumpsolMassphys.massdoublee_MclumpError of clump masssolMassstat.errordoubleLclumpLuminosity of clumpsolLumphys.luminositydoublee_LclumpError of clump luminositysolLumstat.errordoubleL/MRatio of luminosity to masssolLum/solMassphys.luminosityfloate_L/MError of the ratio of luminosity to masssolLum/solMassstat.errorfloatrpcSize of clumppcphys.angSizefloatEccEccentricity of the clumpsrc.orbital.eccentricityfloatVlsrVelocity of the clumpkm/sphys.veloc;pos.lsrfloate_Vlsr? Error of the clump velocitykm/sstat.error;phys.veloc;pos.lsrfloatnullableDistDistance of clump (3)kpcpos.distancefloate_DistError of the distancekpcstat.errorfloatKDAThe ways used to solve the Kinematic Distance Ambiguities (4)meta.codecharSimpleAssThe classification results that describes the association relation between HII regions and high-mass starless clump candidates (5)meta.codecharShapeMore detailed description for the morphology of environment of clump (6)meta.codecharSimbadSimbad column added by the CDSmeta.ref.urlchar_RAPosition from Yuan et al., 2017, Cat. J/ApJS/231/11 (right ascension part)degpos.eq.ra;meta.main_DEPosition from Yuan et al., 2017, Cat. J/ApJS/231/11 (declination part)degpos.eq.dec;meta.main