Journal
ASTRONOMY & ASTROPHYSICS
Volume 533, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201117315
Keywords
dust, extinction; stars: early-type; ISM: structure; stars: protostars; ISM: individual objects: Vela C
Categories
Funding
- CEA/Marie-Curie Eurotalents Fellowship
- ANR (Agence Nationale pour la Recherche) [ANR-08-BLAN-0241]
- CSA (Canada)
- NAOC (China)
- CEA
- ASI (Italy)
- MCINN (Spain)
- SNSB (Sweden)
- STFC (UK)
- NASA (USA)
- BMVIT (Austria)
- ESA-PRODEX (Belgium)
- CEA/CNES (France)
- DLR (Germany)
- ASI/INAF (Italy)
- CNES
- CNRS (France)
- CICYT/MCYT (Spain)
- STFC [PP/D000963/1, ST/G002533/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/D000963/1, ST/G002533/1] Funding Source: researchfish
Ask authors/readers for more resources
We present the first Herschel PACS and SPIRE results of the Vela C molecular complex in the far-infrared and submillimetre regimes at 70, 160, 250, 350, and 500 mu m, spanning the peak of emission of cold prestellar or protostellar cores. Column density and multi-resolution analysis (MRA) differentiates the Vela C complex into five distinct sub-regions. Each sub-region displays differences in their column density and temperature probability distribution functions (PDFs), in particular, the PDFs of the Centre-Ridge and South-Nest sub-regions appear in stark contrast to each other. The Centre-Ridge displays a bimodal temperature PDF representative of hot gas surrounding the HII region RCW36 and the cold neighbouring filaments, whilst the South-Nest is dominated by cold filamentary structure. The column density PDF of the Centre-Ridge is flatter than the South-Nest, with a high column density tail, consistent with formation through large-scale flows, and regulation by self-gravity. At small to intermediate scales MRA indicates the Centre-Ridge to be twice as concentrated as the South-Nest, whilst on larger scales, a greater portion of the gas in the South-Nest is dominated by turbulence than in the Centre-Ridge. In Vela C, high-mass stars appear to be preferentially forming in ridges, i.e., dominant high column density filaments.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available