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Atomic and Molecular Gas in M17 SW

Published online by Cambridge University Press:  21 March 2013

J. P. Pérez-Beaupuits ,
J. Stutzki ,
R. Güsten ,
V. Ossenkopf  and
H. Wiesemeyer
J. P. Pérez-Beaupuits
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: jp@mpifr.de
J. Stutzki
Affiliation:
I. Physikalisches Institut der Universitaet zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
R. Güsten
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: jp@mpifr.de
V. Ossenkopf
Affiliation:
I. Physikalisches Institut der Universitaet zu Köln, Zülpicher Straße 77, 50937 Köln, Germany
H. Wiesemeyer
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: jp@mpifr.de
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Abstract

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We probe the spatial distribution of the [C ii] μm fine-structure emission and its association with neutral and molecular gas in a 5′.7 × 3′.7 (∼3.3 × 2.1 pc2) region of the M17 SW nebula. Comparison of velocity-resolved [C ii] emission maps with other atomic and molecular tracers is possible for the first time with the dual band receiver GREAT on board the SOFIA airborne telescope. We detected [C ii] emission in a much broader velocity range than the CO-lines (Pérez-Beaupuits et al. 2012). Only [C ii] narrow channel maps at intermediate velocities (between 10 and 24 kms) show correlations with other molecular gas components, supporting a clumpy cloud scenario. At lower (< 10 kms) and higher (>24 kms) velocities instead, we see more than 60% of the region mapped in [C ii] that is not associated with other tracers of star-forming material, the so called “CO-dark” gas. Interaction with winds and outflows lead to substantial excitation of [C ii] emitting gas, so that ablation and shock-interaction have to be taken into account to model the observed [C ii] emission.

Keywords

ISM: structure — ISM: atoms — ISM: clouds — ISM: individual (M17)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 55
Copyright
Copyright © International Astronomical Union 2013

References

Pérez-Beaupuits, J. P., Wiesemeyer, H., Ossenkopf, V., Stutzki, J., et al. 2012, A&A, 542, L13Google Scholar