Volume 510, February 2010
|Number of page(s)||12|
|Section||Interstellar and circumstellar matter|
|Published online||16 February 2010|
CHAMP+ observations of warm gas in M 17 SW
Kapteyn Astronomical Institute, Rijksuniversiteit Groningen, 9747 AV Groningen, The Netherlands e-mail: firstname.lastname@example.org
2 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
4 SRON Netherlands Institute for Space Research , PO Box 800, 9700 AV Groningen, The Netherlands
5 Nederlandse Onderzoeksschool Voor Astronomie (NOVA), PO Box 9513, 2300 RA Leiden, The Netherlands
Accepted: 26 October 2009
Context. Sub-millimeter and Far-IR observations have shown the presence of a significant amount of warm (few hundred K) and dense () gas in sources ranging from active star-forming regions to the vicinity of the Galactic center. Since the main cooling lines of the gas phase are important tracers of the interstellar medium in Galactic and extragalactic sources, proper and detailed understanding of their emission and the ambient conditions of the emitting gas, is necessary for a robust interpretation of the observations.
Aims. With high resolution () maps (~ pc2) of mid-J molecular lines we aim to probe the physical conditions and spatial distribution of the warm (50 to several hundred K) and dense gas () across the interface region of the nearly edge-on M 17 SW nebula.
Methods. We have used the dual color multiple pixel receiver CHAMP+ on the APEX telescope to obtain a map of the and transitions of 12CO, the 13CO line, and the 370 μm fine-structure transition of [C I] in M 17 SW. LTE and non-LTE radiative transfer models are used to constrain the ambient conditions.
Results. The warm gas extends up to a distance of ~2.2 pc from the M 17 SW ridge. The 13CO and [C I] 370 μm lines have a narrower spatial extent of about 1.3 pc along a strip line at . The structure and distribution of the [C I] 370 μm map indicate that its emission arises from the interclump medium with densities on the order of .
Conclusions. The warmest gas is located along the ridge of the cloud, close to the ionization front. An LTE approximation indicates that the excitation temperature of the embedded clumps reaches ~120 K. The non-LTE model suggests that the kinetic temperature at four selected positions cannot exceed 230 K in clumps of a density of and that the warm ( K) and dense () gas traced by the mid-J 12CO lines represents just about 2% of the bulk of the molecular gas. The clump volume-filling factor ranges between 0.04 and 0.11 at these positions.
Key words: ISM: general / ISM: atoms / ISM: molecules
© ESO, 2010
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