Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites

Hill, T., Motte, F., Didelon, P., Bontemps, S., Minier, V., Hennemann, M., Schneider, N., André, Ph., Men'shchikov, A., Anderson, L. D., Arzoumanian, D., Bernard, J.-P., Di Francesco, J., Elia, D., Giannini, T., Griffin, Matthew Joseph ORCID: https://orcid.org/0000-0002-0033-177X, Könyves, V., Kirk, Jason M., Marston, A. P., Martin, P. G., Molinari, S., Nguyen Luong, Q., Peretto, Nicolas ORCID: https://orcid.org/0000-0002-6893-602X, Pezzuto, S., Roussel, H., Sauvage, M., Sousbie, T., Testi, L., Ward-Thompson, Derek ORCID: https://orcid.org/0000-0003-1140-2761, White, G. J., Wilson, C. D. and Zavagno, A. 2011. Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites. Astronomy and Astrophysics 533 , A94. 10.1051/0004-6361/201117315

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Abstract

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 μm, 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 RCW 36 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.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	dust, extinction / stars: early-type / ISM: structure / stars: protostars / ISM: individual objects: Vela C
Additional Information:	9 pp. Pdf uploaded in accordance with publisher's policy at http://www.sherpa.ac.uk/romeo/issn/0004-6361/ (accessed 16/04/2014)
Publisher:	EDP Sciences
ISSN:	0004-6361
Date of First Compliant Deposit:	30 March 2016
Last Modified:	23 May 2023 22:06
URI:	https://orca.cardiff.ac.uk/id/eprint/24815

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