Issue |
A&A
Volume 548, December 2012
|
|
---|---|---|
Article Number | L6 | |
Number of page(s) | 6 | |
Section | Letters | |
DOI | https://doi.org/10.1051/0004-6361/201220504 | |
Published online | 27 November 2012 |
Resolving the Vela C ridge with P-ArTéMiS and Herschel⋆,⋆⋆,⋆⋆⋆
1
Laboratoire AIM, CEA/IRFU CNRS/INSU Université Paris Diderot,
CEA-Saclay,
91191
Gif-sur-Yvette Cedex,
France
e-mail: tracey.hill@cea.fr
2
Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud 11,
91405
Orsay,
France
3
Canadian Institute for Theoretical Astrophysics – CITA, University
of Toronto, 60 St. George
Street, Toronto,
Ontario, M5S 3H8, Canada
4
Université de Bordeaux, Bordeaux, LAB, UMR 5804,
33270
Floirac,
France
5
CNRS, LAB, UMR 5804, 33270
Floirac,
France
6
IAPS – Instituto di Astrofisica e Planetologia Spaziali,
via Fosso del Cavaliere
100, 00133
Roma,
Italy
7
European Southern Observatory, Karl Schwarzschild Str. 2, 85748
Garching bei Munchen,
Germany
Received:
5
October
2012
Accepted:
30
October
2012
We present APEX/P-ArTéMiS 450 μm continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel/SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArTéMiS. We extract the radial density profile of the Vela C ridge which with a ~0.1 pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths.
Key words: ISM: individual objects: Vela C / ISM: individual objects: RCW 36 / submillimeter: stars / dust, extinction / stars: early-type / stars: protostars
This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX) in ESO program 083.C-0996. APEX is a collaboration between the Max-Planck-Institut für Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory.
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Figures 4, 5, and Appendix A are available in electronic form at http://www.aanda.org
© ESO, 2012
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