期刊
ASTRONOMY & ASTROPHYSICS
卷 555, 期 -, 页码 -出版社
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201321318
关键词
stars: formation; ISM: kinematics and dynamics; ISM: clouds; stars: massive; ISM: structure
资金
- European Research Council [291294]
- PROBeS
- French National Research Agency (ANR)
- European Community Seventh Framework Programme [229517]
- European ALMA Regional Centre (ARC)
- UK ARC node
- NFS (USA)
- NINS (Japan)
- NRC (Canada)
- NSC
- ASIAA (Taiwan)
- cooperation with the Republic of Chile
- Australian Research Council
- [ANR-11-BS56-010STARFICH]
- STFC [ST/G004633/1, ST/K002465/1, ST/J004502/1, ST/J001562/1, ST/I001425/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/I001425/1, ST/K002465/1, ST/J001562/1, ST/J004502/1, ST/G004633/1] Funding Source: researchfish
- European Research Council (ERC) [291294] Funding Source: European Research Council (ERC)
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-circle dot 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-circle dot contained within a source diameter of 0.05 pc, 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 V-inf = 0.7(+/- 0.2) km s(-1), and a total mass infall rate. M-inf similar or equal to 2.5(+/- 1.0) x 10(-3) Mfi yr(-1) towards the central pc-size region of SDC335. This infall rate brings 750(+/- 300) Mfi of gas to the centre of the cloud per free-fall time (t(ff) = 3 x 10(5) yr). This is enough to double the mass already present in the central pc-size region in 3.5 (+2:2)(-1:0) x t(ff). 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.
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