J/MNRAS/461/2288ivo://CDS.VizieR/J/MNRAS/461/2288doi:10.26093/cds/vizier.74612288CDSHe Y.Zhou J.Esimbek J.Ji W.Wu G.Tang X.Komesh T.Yuan Y.,Li D.Baan W.A.2024-08-16T20:17:46Z2018-02-19T15:49:33ZCDS support team

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

cds-question@unistra.frgalaxiescatalogsmillimeter-astronomysubmillimeter-astronomyspectroscopyradio-astronomyIn this work, we aim to characterize high-mass clumps with infall motions. We selected 327 clumps from the Millimetre Astronomy Legacy Team 90-GHz survey, and identified 100 infall candidates. Combined with the results of He et al. (2015, Cat. J/MNRAS/450/1926), we obtained a sample of 732 high-mass clumps, including 231 massive infall candidates and 501 clumps where infall is not detected. Objects in our sample were classified as pre-stellar, proto-stellar, HII or photodissociation region (PDR). The detection rates of the infall candidates in the pre-stellar, proto-stellar, HII and PDR stages are 41.2 per cent, 36.6 per cent, 30.6 per cent and 12.7 per cent, respectively. The infall candidates have a higher H_2_ column density and volume density compared with the clumps where infall is not detected at every stage. For the infall candidates, the median values of the infall rates at the pre-stellar, proto-stellar, HII and PDR stages are 2.6 x 10^-3^, 7.0x10^-3^, 6.5x10^-3^ and 5.5x10^-3^M_{sun}_/yr, respectively. These values indicate that infall candidates at later evolutionary stages are still accumulating material efficiently. It is interesting to find that both infall candidates and clumps where infall is not detected show a clear trend of increasing mass from the pre-stellar to proto-stellar, and to the HII stages. The power indices of the clump mass function are 2.04+/-0.16 and 2.17+/-0.31 for the infall candidates and clumps where infall is not detected, respectively, which agree well with the power index of the stellar initial mass function (2.35) and the cold Planck cores (2.0).2016MNRAS.461.2288Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/461/2288CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/MNRAS/450/1926 : Infall motions in massive star-forming regions (He+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/461/2288https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/461/2288http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/461/2288https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/461/2288https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/461/2288http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/461/2288GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapRadiodefaultJ/MNRAS/461/2288/tablea1Derived clump parameters (list of He et al., 2015, Cat. J/MNRAS/450/1926)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_Clump[*] * for infall candidates (G1)meta.notecharClumpClump name (GLLL.lll+B.bbb) (G2)meta.id;meta.maincharFpeakPeak submillimetre emissionJy/beamphot.flux.density;em.mm.200-400GHzfloatFintIntegrated submillimetre emissionJyphot.flux.density;em.mm.200-400GHzfloatTdustDust temperatureKphys.temperaturefloatDist? Heliocentric distancekpcpos.distancefloatnullableReff? Effective physical radiuspcphys.size.radiusfloatnullableARAspect ratiosrc.morph.paramfloatlogNH2H_2_ column densitylog(cm**-2)phys.columnDensityfloatlogMclump? Clump mass derived from the integrated 870um emissionlog(solMass)phys.massfloatnullablelogMVir? Virial masslog(solMass)phys.massfloatnullableVDens? Volume density10000cm**-3src.classfloatnullableClassSpitzer classificationsrc.classcharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/MNRAS/461/2288/tablea23Derived clump parameters (table A2) and derived line parameters and profiles of the observed sources (table A3)FpeakPeak submillimetre emissionJy/beamphot.flux.density;em.mm.200-400GHzfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_Clump[*] * for infall candidates (G1)meta.notecharClumpClump name (GLLL.lll+B.bbb) (G2)meta.id;meta.maincharFintIntegrated submillimetre emissionJyphot.flux.density;em.mm.200-400GHzfloatTdustDust temperatureKphys.temperaturefloatDist? Heliocentric distancekpcpos.distancefloatnullabler_Dist? Distance reference (3)meta.ref;pos.frameintnullableReff? Effective physical radiuspcphys.size.radiusfloatnullableARAspect ratiosrc.morph.paramfloatlogNH2H_2_ column densitylog(cm**-2)phys.columnDensityfloatlogMclump? Clump mass derived from the integrated 870um emissionlog(solMass)phys.massfloatnullablelogMvirial? Virial masslog(solMass)phys.massfloatnullableVDens? Volume density10000cm**-3src.classfloatnullableClassSpitzer classificationsrc.classcharVHCO+Peak velocity of HCO^+^(1-0)km/sspect.dopplerVelocfloate_VHCO+rms uncertainty on VHCO+km/sstat.errorfloatVHNCPeak velocity of HNC(1-0)km/sspect.dopplerVelocfloate_VHNCrms uncertainty on VHNCkm/sstat.errorfloatVN2H+Peak velocity of N_2_H^+^(1-0)km/sspect.dopplerVelocfloate_VN2H+rms uncertainty on VN2Hkm/sstat.errorfloatDVN2H+FWHM of N_2_H^+^(1-0)km/sphys.angSizefloate_DVN2H+rms uncertainty on DVN2H+km/sstat.errorfloatdvHCO+Asymmetry of HCO^+^(1-0)spect.line.asymmetryfloatdvHNCAsymmetry of HNC(1-0)spect.line.asymmetryfloatPHCO+[BRN] Profile of HCO^+^(1-0) (3)meta.codecharPHNC[BRN] Profile of HNC(1-0) (3)meta.codecharSimbadSimbad column added by the CDSmeta.ref.urlchar