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Gas and Dust in the Orion Bar

Published online by Cambridge University Press:  25 November 2011

M. Röllig ,
R. Simon ,
V. Ossenkopf ,
J. Stutzki ,
H. Arab ,
M. Compiègne ,
E. Habart  and
A. Abergel
H. Arab
Affiliation:
Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud 11, Orsay, France
M. Compiègne
Affiliation:
Spitzer Science Center, California Institute of Technology, 1200 East California Bd., MC 314-6, Pasadena, CA 91125, USA
E. Habart
Affiliation:
Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud 11, Orsay, France
A. Abergel
Affiliation:
Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud 11, Orsay, France
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Abstract

We use the DustEM model coupled with a radiative transfer code to fit the Herschel and Spitzer emission of the Orion Bar. The thermal dust emission at the 250-μm peak position is well reproduced but we overestimate the stochastically heated grain emission. The dust model parameters are checked with the Meudon PDR code and are consistent with the spectroscopic data from the SPIRE FTS.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 52: Conditions and Impact of Star Formation , 2011 , pp. 277 - 279
Copyright
© EAS, EDP Sciences 2011

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References

Compiègne, M., et al., 2011, A&A, 525, A103
Habart, E., et al., 2010, A&A, 518, L116
Hirota, T., et al., 2007, PASJ, 59, 897H
Le Petit, F., et al., 2006, ApJS, 164, 506L CrossRef
Marconi, A., et al., 1998, A&A, 330, 696