Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites - Archive ouverte HAL Accéder directement au contenu
Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2011

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

Tracey Hill
  • Fonction : Auteur
Pierre Didelon
  • Fonction : Auteur
Martin Hennemann
  • Fonction : Auteur
N. Schneider
  • Fonction : Auteur
Alexander Men'Shchikov
  • Fonction : Auteur
Loren D. Anderson
  • Fonction : Auteur
Doris Arzoumanian
James Di Francesco
Davide Elia
  • Fonction : Auteur
Teresa Giannini
  • Fonction : Auteur
Matt J. Griffin
  • Fonction : Auteur
Jason Kirk
Vera Konyves
  • Fonction : Auteur
Anthony P. Marston
  • Fonction : Auteur
Peter Martin
Sergio Molinari
  • Fonction : Auteur
Quang Nguyen Luong
  • Fonction : Auteur
Nicolas Peretto
  • Fonction : Auteur
Stefano Pezzuto
Marc Sauvage
  • Fonction : Auteur
D. Ward-Thompson
  • Fonction : Auteur

Résumé

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 um, 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.

Dates et versions

hal-00620136 , version 1 (07-09-2011)

Identifiants

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Tracey Hill, Frederique Motte, Pierre Didelon, Sylvain Bontemps, Vincent Minier, et al.. Filaments and ridges in Vela C revealed by Herschel: from low-mass to high-mass star-forming sites. Astronomy and Astrophysics - A&A, 2011, 533, pp.A94. ⟨10.1051/0004-6361/201117315⟩. ⟨hal-00620136⟩
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