J/ApJS/270/9ivo://CDS.VizieR/J/ApJS/270/9doi:10.26093/cds/vizier.22700009CDSXu F.Wang KeLiu T.Tang M.Evans II N.J.Palau A.Morii K.He J.,Sanhueza P.Liu H.-L.Stutz A.Zhang Q.Chen XiLi P.S.Gomez G.C.,Vazquez-Semadeni E.Li S.Mai X.Lu X.Liu M.Chen LiLi C.Shi H.,Ren Z.Li DiGaray G.Bronfman L.Dewangan L.Juvela M.Lee C.W.,Zhang S.Yue N.Wang C.Ge Y.Jiao W.Luo Q.Zhou J.-W.,Tatematsu K.Chibueze J.O.Su K.Sun S.Ristorcelli I.Toth L.V.2024-11-06T20:30:53Z2024-05-13T12:29:57ZCDS support team

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

cds-question@unistra.frinterstellar-mediumstar-forming-regionsradio-astronomymillimeter-astronomysubmillimeter-astronomyco-line-emissionThe Atacama Large Millimeter/submillimeter Array (ALMA) Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE) aims to investigate the process of mass assembly and its connection to high-mass star formation theories in protoclusters in a dynamic view. We observed 11 massive (M_clump_>~10^3^M_{sun}_), luminous (L_bol_>~10^4^L_{sun}_), and blue-profile (infall signature) clumps by ALMA with resolution of ~2200-5500au (median value of 3500au) at 350GHz (870{mu}m). We identified 248 dense cores, including 106 cores showing protostellar signatures and 142 prestellar core candidates. Compared to early stage infrared dark clouds (IRDCs) by ASHES, the core mass and surface density within the ASSEMBLE clumps exhibited a significant increment, suggesting concurrent core accretion during the evolution of the clumps. The maximum mass of prestellar cores was found to be 2 times larger than that in IRDCs, indicating that evolved protoclusters have the potential to harbor massive prestellar cores. The mass relation between clumps and their most massive core (MMCs) is observed in ASSEMBLE but not in IRDCs, which is suggested to be regulated by multiscale mass accretion. The mass correlation between the core clusters and their MMCs has a steeper slope compared to that observed in stellar clusters, which can be due to fragmentation of the MMC and stellar multiplicity. We observe a decrease in core separation and an increase in central concentration as protoclusters evolve. We confirm primordial mass segregation in the ASSEMBLE protoclusters, possibly resulting from gravitational concentration and/or gas accretion.2024ApJS..270....9Xhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/270/9CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)J/A+A/291/943 : Protostellar cores (Ossenkopf+, 1994)J/A+AS/115/81 : A CS(2-1) survey of UC HII regions (Bronfman+, 1996)J/A+A/308/573 : Ammonia on YSOs IRAS sources (Molinari+ 1996)J/A+A/426/97 : SIMBA survey. 1.2-mm/IRAS sources (Faundez+, 2004)J/ApJ/641/389 : Millimetric observations of IRDC cores (Rathborne+, 2006)J/ApJ/651/L125 : Water masers associated with IR cloud cores (Wang+, 2006)J/AJ/136/2391 : GLIMPSE Extended Green Objects catalog (Cyganowski+, 2008)J/A+A/505/405 : A catalogue of Spitzer dark clouds (Peretto+, 2009)J/ApJS/188/123 : The Bolocam Galactic Plane Survey. II. (Rosolowsky+, 2010)J/MNRAS/418/1689 : Red MSX water maser and ammonia emissions (Urquhart+, 2011)J/ApJ/756/60 : A 3mm line survey in 37 IR dark clouds (Sanhueza+, 2012)J/A+A/553/A115 : Millimetric and far-IR maps of IRDC 18310-4 (Beuther+, 2013)J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)J/A+A/561/A83 : SDC13 infrared dark clouds spectra (Peretto+, 2014)J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)J/A+A/577/A30 : SDC335.579-0.292 6, 8, 23 and 25GHz images (Avison+, 2015)J/MNRAS/450/1926 : Infall motions in massive star-forming regions (He+, 2015)J/MNRAS/471/100 : Hi-GAL compact source catalog. -71.0<l<67.0 (Elia+, 2017)J/ApJS/231/11 : High-mass starless clump cand. from ATLASGAL (Yuan+, 2017)J/ApJ/862/105 : Core mass function across Gal. env. II. (Liu+, 2018)J/MNRAS/473/1059 : Complete sample of Galactic clumps (Urquhart+, 2018)J/MNRAS/475/5659 : OB association members (Ward+, 2018)J/ApJ/885/131 : High-mass SFR plx & proper motion with VLBI (Reid+, 2019)J/ApJ/886/102 : ALMA obs. of 70um high-mass clumps (ASHES) (Sanhueza+, 2019)J/MNRAS/496/2790 : ATOMS I and a first look at G9.62+0.19 (Liu+, 2020)J/ApJ/912/156 : Core kinematics in the Dragon IRDC from ALMA (Kong+, 2021)J/ApJS/259/36 : Filaments in the inner Gal. plane from ATLASGAL (Ge+, 2022)J/A+A/657/A30 : W51 North ALMA 1.3 and 3mm images (Tang+, 2022)J/A+A/674/A75 : W43-MM1 and W43-MM2+MM3 ALMA datacubes (Nony+, 2023)J/ApJS/264/35 : C^18^O dense cores in Orion A (Takemura+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/270/9https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/270/9http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/270/9https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/270/9https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/270/9http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/270/9GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJS/270/9/table1 (Physical properties of the ASSEMBLE clumps)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/270/9/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/270/9/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/270/9/table1?GETtext/xml+votable180.050000true220.5115-60.509750.005555555555555556Cone search capability for table J/ApJS/270/9/cores (Fundamental measurements and calculated properties of the cores identified with the getsf algorithm (Tables 3 and 4))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/270/9/cores?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/270/9/cores?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/270/9/cores?GETtext/xml+votable180.050000true220.5079583-60.50269440.0055555555555555566/41763 41778 42159 42211 42224 42450-42451 42497-42498https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJS/270/9?format=asciiMillimeterRadiodefaultJ/ApJS/270/9/table1Physical properties of the ASSEMBLE clumpsSimbadNameSimbad column added by the CDSmeta.idcharnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNcNumber of cores identified in this clumpmeta.numberintnullableIRNameIRAS name (IHHMMm+DDMM; B1950)meta.id.assoccharAGALAGAL identifier (GLLL.lll+BB.bbb) from Urquhart+ (2018, J/MNRAS/473/1059)meta.id;meta.maincharRAJ2000Hour of right ascension (J2000) (1)pos.eq.ra;meta.mainDEJ2000Degree of declination (J2000) (1)pos.eq.dec;meta.mainVlsr[-95/-17.7] Local Standard of Rest velocity derived from the CO(4-3) and C^17^O(3-2) lines in APEX obs. (Yue+ 2021RAA....21...14Y)km/sphys.veloc;pos.lsrfloate_Vlsr[-0.9/-0.4] Vlsr uncertaintykm/sstat.error;phys.veloc;pos.lsrfloatDist[2.5/7.6] Distance (2)kpcpos.distancefloate_Dist[0.18/0.7] Lower uncertainty on Dist (2)kpcstat.errorfloatE_Dist[0.3/0.7] Upper uncertainty on Dist (2)kpcstat.error;stat.maxfloatRcl[0.16/0.8] Radius derived from 2D Gaussian fitting; in parsec (3)pcphys.size.radiusfloatRad[12/28] Radius derived from 2D Gaussian fitting; in arcsec (3)arcsecphys.angSize;srcintTdust[23/32.2] Clump dust temperature (4)Kphys.temperaturefloatlogM[2.8/4.4] Log of clump mass (4)log(solMass)phys.massfloatlogLbol[4/6] Log of clump bolometric luminosity (4)log(solLum)phys.luminosityfloatL/M[11/79] Luminosity-to-mass ratio (4)solLum/solMassphys.composition.massLightRatiointSigma[0.7/6.5] Clump surface density ({Sigma}_cl_=M_cl_/({pi}R_cl_^2^))g.cm**-2phot.flux.density.sbfloatIDClump ID as in tables 3 and 4; column added by CDS (IHHMMm)meta.idcharprimaryATLASGALDisplay data from Urquhart+ 2014, J/A+A/568/A41meta.ref.urlcharJ/ApJS/270/9/coresFundamental measurements and calculated properties of the cores identified with the getsf algorithm (Tables 3 and 4)Core[1/37] Core ID (1)meta.id.part;meta.mainintIDASSEMBLE clump (IHHMMm)meta.id.parentcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000[14/17] Hour of right ascension (J2000) (2)pos.eq.ra;meta.mainDEJ2000[36/60] Degree of declination (J2000) (2)pos.eq.dec;meta.mainIpeak[2.8/1970] Peak intensitymJy/beamspect.line.intensityfloate_Ipeak[0.3/129] Uncertainty on IpeakmJy/beamstat.errorfloatFlux[7.6/5133] Integrated fluxmJyphot.flux.density;em.mm.200-400GHzfloate_Flux[0.3/139] Uncertainty on FluxmJystat.error;phot.fluxfloatFWHM-maj[0.79/5.4] Fitted FWHM of major axis convolved with beamarcsecphys.angSize;instr.beamfloatFWHM-min[0.5/3.5] Fitted FWHM of minor axis convolved with beamarcsecphys.angSize;instr.beamfloatPAPosition Angle measured anticlockwise from northdegpos.posAngfloatFWHM-c[0.7/4.3] Deconvolved FWHM of core sizearcsecphys.angSizefloatClass[0/5] Core classification based on Section 4.3 (3)meta.code.classintTdust[23/183] Dust temperatureKphys.temperatureinte_Tdust[1/27] Uncertainty on TdustKstat.errorintMethDust temperature estimation method (1)meta.codecharMcore[0.1/53] Mass of coresolMassphys.massfloate_Mcore[0.1/23] Uncertainty on McoresolMassstat.errorfloatRcore[1050/14620] Radius of coreauphys.size.radiusintnH2[0.01/352] H2 volume density1e+06cm**-3phys.densityfloate_nH2[0.01/159] Uncertainty on nH21e+06cm**-3stat.errorfloatSigma[0.1/12] Surface densityg.cm**-2src.densityfloate_Sigma[0.06/5] Uncertainty on Sigmag.cm**-2stat.errorfloatNpeak[0.2/25.3] H2 peak column density1e+23cm**-2phys.columnDensity;stat.maxfloate_Npeak[0.1/9] Uncertainty on Npeak1e+23cm**-2stat.errorfloat