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Dense cores and star formation in the giant molecular cloud Vela C
- Source :
- Astronomy and Astrophysics-A&A, Astronomy and Astrophysics-A&A, EDP Sciences, 2019, 628, pp.A110. ⟨10.1051/0004-6361/201935047⟩, Astronomy and Astrophysics-A&A, 2019, 628, pp.A110. ⟨10.1051/0004-6361/201935047⟩
- Publication Year :
- 2019
- Publisher :
- HAL CCSD, 2019.
-
Abstract
- Context The Vela Molecular Ridge is one of the nearest (700 pc) giant molecular cloud (GMC) complexes hosting intermediate-mass (up to early B, late O stars) star formation, and is located in the outer Galaxy, inside the Galactic plane. Vela C is one of the GMCs making up the Vela Molecular Ridge, and exhibits both sub-regions of robust and sub-regions of more quiescent star formation activity, with both low- and intermediate(high)-mass star formation in progress. Aims We aim to study the individual and global properties of dense dust cores in Vela C, and aim to search for spatial variations in these properties which could be related to different environmental properties and/or evolutionary stages in the various sub-regions of Vela C. Methods We mapped the submillimetre (345 GHz) emission from vela C with LABOCA (beam size 19.2", spatial resolution ~0.07 pc at 700 pc) at the APEX telescope. We used the clump-finding algorithm CuTEx to identify the compact submillimetre sources. We also used SIMBA (250 GHz) observations, and Herschel and WISE ancillary data. The association with WISE red sources allowed the protostellar and starless cores to be separated, whereas the Herschel dataset allowed the dust temperature to be derived for a fraction of cores. The protostellar and starless core mass functions (CMFs) were constructed following two different approaches, achieving a mass completeness limit of 3.7 Msun. Results We retrieved 549 submillimetre cores, 316 of which are starless and mostly gravitationally bound (therefore prestellar in nature). Both the protostellar and the starless CMFs are consistent with the shape of a Salpeter initial mass function in the high-mass part of the distribution. Clustering of cores at scales of 1--6 pc is also found, hinting at fractionation of magnetised, turbulent gas.<br />Comment: 21 pages, 19 figures, to be published in Astronomy & Astrophysics
- Subjects :
- Initial mass function
FOS: Physical sciences
Context (language use)
Astrophysics
Vela
01 natural sciences
0103 physical sciences
protostar [Stars]
individual objects: Vela Molecular Ridge [ISM]
010303 astronomy & astrophysics
Solar and Stellar Astrophysics (astro-ph.SR)
formation [Stars]
ComputingMilieux_MISCELLANEOUS
O-type star
Physics
[PHYS]Physics [physics]
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
010308 nuclear & particles physics
Star formation
Molecular cloud
ISM [Submillimeter]
Astronomy and Astrophysics
Galactic plane
Astrophysics - Astrophysics of Galaxies
Galaxy
Astrophysics - Solar and Stellar Astrophysics
13. Climate action
Space and Planetary Science
Astrophysics of Galaxies (astro-ph.GA)
structure [ISM]
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Subjects
Details
- Language :
- English
- ISSN :
- 00046361
- Database :
- OpenAIRE
- Journal :
- Astronomy and Astrophysics-A&A, Astronomy and Astrophysics-A&A, EDP Sciences, 2019, 628, pp.A110. ⟨10.1051/0004-6361/201935047⟩, Astronomy and Astrophysics-A&A, 2019, 628, pp.A110. ⟨10.1051/0004-6361/201935047⟩
- Accession number :
- edsair.doi.dedup.....7376e9102781ffb02cebbed0d2374c4e