J/MNRAS/508/2964ivo://CDS.VizieR/J/MNRAS/508/2964doi:10.26093/cds/vizier.75082964CDSAnderson M.Peretto N.Ragan S.E.Rigby A.J.Avison A.,Duarte-Cabral A.Fuller G.A.Shirley Y.L.Traficante A.Williams G.M.2025-07-18T20:17:07Z2024-09-12T13:59:47ZCDS support team

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

cds-question@unistra.frstar-forming-regionsmolecular-cloudsastrometryinfrared-astronomyradio-sourcesmillimeter-astronomysubmillimeter-astronomyphotometryclassificationThe physical processes behind the transfer of mass from parsec-scale clumps to massive star-forming cores remain elusive. We investigate the relation between the clump morphology and the mass fraction that ends up in its most massive core (MMC) as a function of infrared brightness, i.e. a clump evolutionary tracer. Using Atacama Large Millimeter/submillimeter Array (ALMA) 12 m and Atacama Compact Array, we surveyed six infrared dark hubs in 2.9 mm continuum at ~3 arcsec resolution. To put our sample into context, we also re-analysed published ALMA data from a sample of 29 high-mass surface density ATLASGAL sources. We characterize the size, mass, morphology, and infrared brightness of the clumps using Herschel and Spitzer data. Within the six newly observed hubs, we identify 67 cores, and find that the MMCs have masses between 15 and 911 M_{sun}_ within a radius of 0.018-0.156 pc. The MMC of each hub contains 3-24 per cent of the clump mass (fMMC), becoming 5-36 per cent once core masses are normalized to the median core radius. Across the 35 clumps, we find no significant difference in the median fMMC values of hub and non-hub systems, likely the consequence of a sample bias. However, we find that fMMC is ~7.9 times larger for infrared dark clumps compared to infrared bright ones. This factor increases up to ~14.5 when comparing our sample of six infrared dark hubs to infrared bright clumps. We speculate that hub-filament systems efficiently concentrate mass within their MMC early on during its evolution. As clumps evolve, they grow in mass, but such growth does not lead to the formation of more massive MMCs.2021MNRAS.508.2964Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/508/2964CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/561/A83 : SDC13 infrared dark clouds spectra (Peretto+, 2014)J/A+A/505/405 : A catalogue of Spitzer dark clouds (Peretto+, 2009)J/A+A/590/A72 : Herschel counterparts of SDC (Peretto+, 2016)J/A+A/591/A149 : Hi-GAL. inner Milky Way: +68>=l>=70 (Molinari+, 2016)J/A+A/600/L10 : Massive cluster progenitors from ATLASGAL (Csengeri+, 2017)J/MNRAS/422/3178 : Distances of 793 BGPS sources (Eden+, 2012)J/A+A/642/A87 : Hub-filament candidates (Kumar+, 2020)J/ApJ/783/130 : Parallaxes of high mass star forming regions (Reid+, 2014)J/ApJS/179/249 : Low-luminosity embedded protostar population (Dunham+, 2008)J/A+A/547/A49 : Herschel EPoS: high-mass overview (Ragan+, 2012)J/MNRAS/471/100 : Hi-GAL compact source catalog. -71.0<l<67.0 (Elia+, 2017)J/A+A/487/993 : MAMBO Mapping of c2d Clouds and Cores (Kauffmann+, 2008)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/508/2964https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/508/2964http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/508/2964https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/508/2964https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/508/2964http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/508/2964GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/508/2964/a2021 (Our clump and core properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/2964/a2021?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/2964/a2021?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/2964/a2021?GETtext/xml+votable180.050000true235.8007914-54.11455360.005555555555555556Cone search capability for table J/MNRAS/508/2964/cores (*Cores properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/2964/cores?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/2964/cores?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/2964/cores?GETtext/xml+votable180.050000true283.31779061.25261220.005555555555555556Cone search capability for table J/MNRAS/508/2964/mmcs (Clump classifications and MMCs properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/508/2964/mmcs?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/508/2964/mmcs?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/508/2964/mmcs?GETtext/xml+votable180.050000true283.31614861.25434640.0055555555555555566/28808 30318-30319 41780 41802 41804 41817 41820 41824 42172 42207 42211-42212 42214 42225 42228-42230 42376 42381 42387 42392 42396 42436 42441 42456-42457 42496-42497https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/508/2964?format=asciiInfraredMillimeterRadiodefaultJ/MNRAS/508/2964/a2021Our clump and core propertiesdEstimated distance (d) (G4)pcpos.distanceintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_dMean error on d (d_err)pcstat.errorintMclumpMass of the clump (M_clump) (G5)solMassphys.massfloatCoreCore name from Galactic coordinates of the clump (LLL.llll+B.bbbb-MMNN) and a number between 1 and 19 (core_name)meta.id;meta.maincharRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (Dec)degpos.eq.dec;meta.mainSnuIntegrated flux density of the source around 2890 {mu}m (S_{nu}_) (G6)Jyphot.flux.density;em.mm.100-200GHzdoubleSnuclipIntegrated flux density of the source with the clipped paradigm around 2890 {mu}m (S_{nu}_clip) (G6)Jyphot.flux.density;em.mm.100-200GHzdoublee_SnuMean error on S_{nu}_ (S_{nu}_err)Jystat.errordoubleInupeakIntegrated flux density of the source pear beam size around 2890 {mu}m (18 pixels) (Inu_peak)Jy/beamphot.flux.density;em.mm.100-200GHzdoubleSNRSignal to noise ratio calculated at the maximum peak values (peak_snr)stat.snr;meta.modelleddoubleBeamFWHMFWHM of the beam area (beam_FWHM) (G7)degphys.angSize;srcdoubleAcoreSize of the core in the square degrees unit 1deg^2^=({pi}/180)^2^sr (A_core)deg**2phys.angSizedoubleReqEquivalent radius (R_eq) (G8)pcphys.size.radiusfloatRsourceDeconvolved source radius (R_source) (G9)pcphys.size.radiusfloatf_Rsource[0/1] Flag on Rsource, 1 for the resolved sources (resolved) (G9)meta.codeintTcolFirst estimated temperature (T_col_) (G10)Kphys.temperaturefloate_Tcol[0.5] Mean error on Tcol (T_col_err)Kstat.errorfloat70um[0/1] Availability of an associated 70 {mu}m source, 1 if it's the case (70micron) (G11)meta.codeintTd? Second estimated temperature (T_d_) (G12)Kphys.temperaturefloatnullablee_Td? Mean error on Td (T_d_err)Kstat.errorfloatnullableTcoreEstimated core temperature (T_core_) (G13)Kphys.temperaturefloate_TcoreMean error on Tcore (T_err)Kstat.errorfloatMcoreCore mass (M_core_) (G14)solMassphys.massdoubleE_McoreMcore error upper value (M_err_pos) (G15)solMassstat.error;stat.maxdoublee_McoreMcore error lower value (M_err_neg) (G15)solMassstat.errordoubleClumpClump name from Galactic coordinates (GLLL.llll+B.bbbb) (clump_name) (G3)meta.id.parentcharJ/MNRAS/508/2964/cores*Cores propertiesReqEquivalent radius (R_eq_) (G8)pcphys.size.radiusfloatSnuIntegrated flux density of the source around 878 {mu}m (S_{nu}_) (G6)Jyphot.flux.density;em.mm.100-200GHzdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFreqObserved frequency (nu) (G2)Hzem.freqdoubleBeamFWHMFWHM of the beam area (beam_FWHM)arcsecphys.angSize;srcfloatdEstimated distance (d) (G4)pcpos.distanceintMclump? Mass of the clump (M_clump) (G5)solMassphys.massfloatnullableRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (Dec)degpos.eq.dec;meta.mainSnuclipIntegrated flux density of the source with the clipped paradigm around 878 {mu}m (S_{nu}_clip) (G6)Jyphot.flux.density;em.mm.100-200GHzdoubleRsourceDeconvolved source radius (R_source_) (G9)pcphys.size.radiusfloatf_Rsource[0/1] Flag on Rsource, 1 for the resolved sources (resolved) (G9)meta.codeintTcol? First estimated temperature (T_col_) (G10)Kphys.temperaturefloatnullable70um[0/1] Availability of an associated 70 {mu}m source, 1 if it's the case (70micron) (G11)meta.codeintTd? Second estimated temperature (T_d_) (G12)Kphys.temperaturefloatnullableTcore? Estimated core temperature (T_core_) (G13)Kphys.temperaturefloatnullableMcore? Core mass (M_core_) (G14)solMassphys.massdoublenullableClumpClump name from Galactic coordinates (GLLL.llll+B.bbbb) (clump_name)meta.id.parentcharSample[C2017/A2021] sample origin (sample) (G1)meta.ref;src.samplecharCoreCore name from Galactic coordinates of the clump (LLL.llll+B.bbbb-MMNN) and a number between 1 and 19 (core_name)meta.id;meta.maincharJ/MNRAS/508/2964/mmcsClump classifications and MMCs propertiesClumpID[1-35] Clump identifier number (clump_ID)meta.idintFreqObserved frequency (nu) (G2)Hzem.freqdoubleRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (Dec)degpos.eq.dec;meta.maindEstimated distance (d) (G4)pcpos.distanceintReqEquivalent radius (R_eq) (G8)pcphys.size.radiusfloatRsourceDeconvolved source radius (R_source) (G9)pcphys.size.radiusfloatTcolFirst estimated temperature (T_col) (G10)Kphys.temperaturefloat70um[0-1] Availability of an associated 70 {mu}m source, 1 if it's the case (70micron) (G11)meta.codeintTd? Second estimated temperature (T_d) (G12)Kphys.temperaturefloatnullableTcoreEstimated core temperature (T_core) (G13)Kphys.temperaturefloatMcoreCore mass (M_core) (G14)solMassphys.massdoubleMclumpMass of the clump (M_clump) (G5)solMassphys.massdoublefMMCThe fraction of the clump mass contained within its MMC (f_MMC) (1)phys.massfloatCFEThe core formation efficiency (CFE) (2)phys.massfloatHFSHubs filament system classification (HFS) (4)src.classintIRclassBrightness category (IR_class) (3)src.classfloatSample[C2017/A2021] sample origin (sample) (G1)meta.ref;src.samplecharCoreCore name from Galactic coordinates of the clump (LLL.llll+B.bbbb-MMNN) and a number between 1 and 19 (core_name)meta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintClumpClump name from Galactic coordinates (GLLL.llll+B.bbbb) (clump_name)meta.id.parentchar