Volume 488, Number 2, September III 2008
|Page(s)||623 - 634|
|Section||Interstellar and circumstellar matter|
|Published online||09 July 2008|
A clumpy-cloud photon-dominated regions model of the global far-infrared line emission of the Milky Way
I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany e-mail: firstname.lastname@example.org
2 SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
3 Argelander Institut für Radioastronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
Accepted: 7 July 2008
Context. The fractal structure of the interstellar medium suggests that the interaction of UV radiation with the ISM as described in the context of photon-dominated regions (PDR) dominates most of the physical and chemical conditions, and hence the far-infrared and submm emission from the ISM in the Milky Way.
Aims. We investigate to what extent the Galactic FIR line emission of the important species CO, C, C+, and O, as observed by the Cosmic Background Explorer (COBE) satellite can be modeled in the framework of a clumpy, UV-penetrated cloud scenario.
Methods. The far-infrared line emission of the Milky Way is modeled as the emission from an ensemble of clumps with a power law clump mass spectrum and mass-size relation with power-law indices consistent with the observed ISM structure. The individual clump line intensities are calculated using the KOSMA-τ PDR-model for spherical clumps. The model parameters for the cylindrically symmetric Galactic distribution of the mass density and volume filling factor are determined by the observed radial distributions. A constant FUV intensity, in which the clumps are embedded, is assumed.
Results. We show that this scenario can explain, without any further assumptions and within a factor of about 2, the absolute FIR-line intensities and their distribution with Galactic longitude as observed by COBE.
Key words: ISM: clouds / Galaxy: disk / infrared: ISM / infrared: galaxies / submillimeter / ISM: structure
© ESO, 2008
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