2024ApJS..270....9X

Query : 2024ApJS..270....9X

2024ApJS..270....9X - Astrophys. J., Suppl. Ser., 270, 9 (2024/January-0)

The ALMA Survey of Star Formation and Evolution in Massive Protoclusters with Blue Profiles (ASSEMBLE): Core Growth, Cluster Contraction, and Primordial Mass Segregation.

XU F., WANG K., LIU T., TANG M., EVANS II N.J., PALAU A., MORII K., HE J., SANHUEZA P., LIU H.-L., STUTZ A., ZHANG Q., CHEN X., LI P.S., GOMEZ G.C., VAZQUEZ-SEMADENI E., LI S., MAI X., LU X., LIU M., CHEN L., LI C., SHI H., REN Z., LI D., GARAY 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. and TOTH L.V.

Abstract (from CDS):

The 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 (Mclump ≳ 103M⊙), luminous (Lbol ≳ 104L⊙), and blue-profile (infall signature) clumps by ALMA with resolution of ∼2200-5500 au (median value of 3500 au) at 350 GHz (870 μm). 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.

Abstract Copyright: © 2023. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Protoclusters - Star formation - Massive stars - Interstellar medium - Protostars - Star forming regions

VizieR on-line data: <Available at CDS (J/ApJS/270/9): table1.dat table3.dat table4.dat>

Simbad objects: 39

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Number of rows : 39
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 LDN 1495 DNe 04 18.1 +27 37           ~ 408 1
2 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4971 0
3 NAME OMC 1S PoC 05 35 14.5 -05 25 49           ~ 78 1
4 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1227 1
5 QSO B1424-41 Bla 14 27 56.29756617 -42 06 19.4376238   18.48 17.7 16.30   ~ 547 1
6 [BNM96] 316.139-0.503 HII 14 42 01.8038893992 -60 30 09.662138316           ~ 29 0
7 AGAL G316.139-00.506 smm 14 42 03 -60 30.6           ~ 15 0
8 IRAS 14498-5856 HII 14 53 42.324 -59 08 57.44           ~ 38 0
9 AGAL G318.049+00.086 cor 14 53 42.427 -59 08 52.75           ~ 18 0
10 ESO 514-1 BLL 15 17 41.8134049824 -24 22 19.482207024   15.13 14.00 13.95   ~ 815 3
11 PKS 1520-58 Rad 15 24 51.12282 -59 03 39.7182           ~ 24 0
12 IRAS 15520-5234 HII 15 55 48.336 -52 43 10.20           ~ 59 1
13 AGAL G328.809+00.632 cor 15 55 49 -52 43.1           ~ 27 0
14 IRAS 15596-5301 HII 16 03 31.800 -53 09 24.48           ~ 33 0
15 [GMB2007b] J160332.1-530928 smm 16 03 32.1 -53 09 28           ~ 17 1
16 MMB G330.953-00.182 cor 16 09 52.37 -51 54 57.6           ~ 40 0
17 IRAS 16060-5146 HII 16 09 52.776 -51 54 52.20           ~ 44 0
18 AGAL G331.133-00.244 cor 16 10 59.590 -51 50 23.37           ~ 25 0
19 IRAS 16071-5142 HII 16 11 00 -51 50.3           ~ 40 0
20 GAL 331.28-00.19 HII 16 11 26.6 -51 41 57           ~ 56 0
21 AGAL G331.279-00.189 cor 16 11 26.748 -51 41 56.04           ~ 22 0
22 [GMB2007b] J163058.7-484353 smm 16 30 58.7 -48 43 53           ~ 26 1
23 IRAS 16272-4837 HII 16 30 59.2 -48 43 48           ~ 42 0
24 AGAL G337.406-00.402 cor 16 38 51 -47 27.9           ~ 26 0
25 IRAS 16351-4722 HII 16 38 52.032 -47 28 11.28           ~ 37 0
26 ICRF J165016.6-504448 QSO 16 50 16.62710806 -50 44 48.2106956   20.95       ~ 89 2
27 IRAS 17204-3636 HII 17 23 49.8 -36 38 47           ~ 20 0
28 AGAL G351.041-00.336 cor 17 23 50.280 -36 38 57.14           ~ 18 0
29 GAL 351.58-00.35 HII 17 25 25.2 -36 12 46           ~ 40 0
30 MMB G351.581-00.353 cor 17 25 25.220 -36 12 45.34           ~ 44 0
31 PMN J1733-3722 Rad 17 33 15.1930935 -37 22 32.398009           ~ 56 1
32 GAL 009.62+00.19 HII 18 06 13.9 -20 31 44           ~ 226 0
33 NAME Aql Region reg 18 31.1 -02 10           ~ 456 0
34 NAME Dragon Nebula DNe 18 42 50.6 -04 03 30           ~ 177 0
35 W 43 SFR 18 47 32 -01 56.5           ~ 604 0
36 AGAL G030.818-00.056 cor 18 47 47.0 -01 54 28           ~ 186 0
37 NAME Corona Australis Cloud MoC 19 01 51 -36 58.9           ~ 554 0
38 NAME W 51 North Rad 19 23 40.0 +14 30 51           ~ 169 0
39 QSO B1921-293 BLL 19 24 51.05595254 -29 14 30.1210248   18.71 18.21 15.07   ~ 918 1

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