2016MNRAS.457.4536W


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.22CEST22:10:32

2016MNRAS.457.4536W - Mon. Not. R. Astron. Soc., 457, 4536-4545 (2016/April-3)

Comparing young massive clusters and their progenitor clouds in the Milky Way.

WALKER D.L., LONGMORE S.N., BASTIAN N., KRUIJSSEN J.M.D., RATHBORNE J.M., GALVAN-MADRID R. and LIU H.B.

Abstract (from CDS):

Young massive clusters (YMCs) have central stellar mass surface densities exceeding 104 M pc–2. It is currently unknown whether the stars formed at such high (proto)stellar densities. We compile a sample of gas clouds in the Galaxy which have sufficient gas mass within a radius of a few parsecs to form a YMC, and compare their radial gas mass distributions to the stellar mass distribution of Galactic YMCs. We find that the gas in the progenitor clouds is distributed differently than the stars in YMCs. The mass surface density profiles of the gas clouds are generally shallower than the stellar mass surface density profiles of the YMCs, which are characterized by prominent dense core regions with radii ∼0.1 pc, followed by a power-law tail. On the scale of YMC core radii, we find that there are no known clouds with significantly more mass in their central regions when compared to Galactic YMCs. Additionally, we find that models in which stars form from very dense initial conditions require surface densities that are generally higher than those seen in the known candidate YMC progenitor clouds. Our results show that the quiescent, less evolved clouds contain less mass in their central regions than in the highly star-forming clouds. This suggests an evolutionary trend in which clouds continue to accumulate mass towards their centres after the onset of star formation. We conclude that a conveyor-belt scenario for YMC formation is consistent with the current sample of Galactic YMCs and their progenitor clouds.

Abstract Copyright: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: formation - ISM: clouds - Galaxy: centre - Galaxy: disc - open clusters and associations: general

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 942 3
2 RMC 136 Cl* 05 38 42.396 -69 06 03.36   9.63 9.50     ~ 1674 2
3 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 412 0
4 NGC 3603 HII 11 15 24 -61 15.0           ~ 920 2
5 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 442 0
6 MMB G350.116+00.084 cor 17 19 28.83 -37 10 18.8           ~ 13 0
7 OH 351.77 -0.54 cor 17 26 42.57 -36 09 17.6           ~ 80 0
8 MMB G352.624-01.077 Mas 17 31 15.31 -35 44 47.7           ~ 8 0
9 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11007 0
10 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 611 0
11 NAME the Brick MoC 17 46 09.7 -28 43 31           ~ 128 0
12 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 424 0
13 NAME Sgr B2 (North) Rad 17 47 20.2 -28 22 21           ~ 493 1
14 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1851 1
15 NAME Sgr B2 Main Rad 17 47 20.5 -28 23 06           ~ 321 1
16 GAL 010.472+00.026 mm 18 08 38 -19 51.9           ~ 2 0
17 BGPS G043.169+00.009 cor 19 10 14.2145 +09 06 17.697           ~ 20 0
18 W 49 SFR 19 10 20 +09 07.7           ~ 502 1
19 W 51 SNR 19 23 50 +14 06.0           ~ 1119 1
20 NGC 7252 IG 22 20 44.7751096408 -24 40 41.905677809 12.26 12.46 12.06 11.57   ~ 655 1
21 NAME Galactic Bar reg ~ ~           ~ 816 0

    Equat.    Gal    SGal    Ecl

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2019.10.22-22:10:32

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