| Issue |
A&A
Volume 539, March 2012
|
|
|---|---|---|
| Article Number | A116 | |
| Number of page(s) | 19 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201118061 | |
| Published online | 02 March 2012 | |
The Carina Flare
What can fragments in the wall tell us?⋆,⋆⋆
1 Astronomical Institute, Academy of Sciences of the Czech
Republic, Bocni II 1401–2a, Prague, Czech Republic
e-mail: richard@wunsch.cz
2
Excellence Cluster “Universe”, Boltzmannstr. 2, 85748
Garching,
Germany
3
School of Mathematics and Physics, University of
Tasmania, Sandy Bay Campus,
Churchill Avenue, Sandy
Bay, TAS
7005,
Australia
4
Department of Physics and Astrophysics, Nagoya
University, Chikusa-ku, Nagoya, Japan
Received: 9 September 2011
Accepted: 18 December 2011
13CO(J = 2–1) and C18O(J = 2–1) observations of the molecular cloud G285.90+4.53 (Cloud 16) in the Carina Flare supershell (GSH287+04-17) with the APEX telescope are presented. With an algorithm DENDROFIND we identify 51 fragments and compute their sizes and masses. We discuss their mass spectrum and interpret it as being the result of the shell fragmentation process described by the pressure assisted gravitational instability – PAGI. We conclude that the explanation of the clump mass function needs a combination of gravity with pressure external to the shell.
Key words: ISM: molecules / stars: formation / stars: winds, outflows / Galaxy: structure / ISM: structure
Based on observations made with ESO telescopes at La Silla Paranal Observatory under programme ID 086.c-0187.
Appendix B is available in electronic form at http://www.aanda.org
© ESO, 2012
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