2013A&A...555A.112P


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.09CET22:30:44

2013A&A...555A.112P - Astronomy and Astrophysics, volume 555A, 112-112 (2013/7-1)

Global collapse of molecular clouds as a formation mechanism for the most massive stars.

PERETTO N., FULLER G.A., DUARTE-CABRAL A., AVISON A., HENNEBELLE P., PINEDA J.E., ANDRE P., BONTEMPS S., MOTTE F., SCHNEIDER N. and MOLINARI S.

Abstract (from CDS):

The relative importance of primordial molecular cloud fragmentation versus large-scale accretion still remains to be assessed in the context of massive core/star formation. Studying the kinematics of the dense gas surrounding massive-star progenitors can tell us the extent to which large-scale flow of material impacts the growth in mass of star-forming cores. Here we present a comprehensive dataset of the 5500(±800)M infrared dark cloud SDC335.579-0.272 (hereafter SDC335), which exhibits a network of cold, dense, parsec-long filaments. Atacama Large Millimeter Array (ALMA) Cycle 0 observations reveal two massive star-forming cores, MM1 and MM2, sitting at the centre of SDC335 where the filaments intersect. With a gas mass of 545(+770–385)M contained within a source diameter of 0.05pc, MM1 is one of the most massive, compact protostellar cores ever observed in the Galaxy. As a whole, SDC335 could potentially form an OB cluster similar to the Trapezium cluster in Orion. ALMA and Mopra single-dish observations of the SDC335 dense gas furthermore reveal that the kinematics of this hub-filament system are consistent with a global collapse of the cloud. These molecular-line data point towards an infall velocity Vinf=0.7(±0.2)km/s, and a total mass infall rate {dot}(M)inf≃2.5(±1.0)x10–3M/yr towards the central pc-size region of SDC335. This infall rate brings 750(±300)M of gas to the centre of the cloud per free-fall time (tff=3x105yr). This is enough to double the mass already present in the central pc-size region in 3.5+2.2–1.0xtff. These values suggest that the global collapse of SDC335 over the past million year resulted in the formation of an early O-type star progenitor at the centre of the cloud's gravitational potential well.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: kinematics and dynamics - ISM: clouds - stars: massive - ISM: structure

Nomenclature: Fig. 1a: [PFD2013] FN (Nos F1-F7). Fig. 1c: [PFD2013] MMN (Nos MM1-MM2).

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1436 1
2 ICRF J160431.0-444131 Bla 16 04 31.02069 -44 41 31.9742   20.75       ~ 55 0
3 [PFD2013] F6 ? 16 29 30.0 -48 44 00           ~ 1 0
4 [PFD2013] F5 ? 16 30 30.0 -48 45 00           ~ 1 0
5 [PFD2013] F1 ? 16 30 30.0 -48 41 00           ~ 1 0
6 [PFD2013] MM2 cor 16 30 57.26 -48 43 39.7           ~ 2 0
7 SDC G335.579-0.292 DNe 16 30 58.00 -48 44 16.3           ~ 22 0
8 [PFD2013] MM1 cor 16 30 58.76 -48 43 53.4           ~ 5 0
9 [PFD2013] F4 ? 16 31 20.0 -48 45 00           ~ 1 0
10 [PFD2013] F3 ? 16 31 30.0 -48 44 20           ~ 1 0
11 [PFD2013] F2 ? 16 31 35.0 -48 43 30           ~ 1 0
12 NAME W 51 North Rad 19 23 40.0 +14 30 51           ~ 140 0
13 NAME Cyg X Cld 20 28 41 +41 10.2           ~ 591 1
14 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 932 0

    Equat.    Gal    SGal    Ecl

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2019.12.09-22:30:44

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