Starburst Models For FIR/sub-mm/mm Line Emission. I. An Expanding Supershell Surrounding A Massive Star Cluster

Abstract

The effect of a newly born star cluster inside a giant molecular cloud (GMC) is to produce a hot bubble and a thin, dense shell of interstellar gas and dust swept up by the H II expansion, strong stellar winds, and repeated supernova explosions. Lying at the inner side of the shell is the photodissociation region (PDR), the origin of much of the far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) radiation from the interstellar medium (ISM). We present a model for the expanding shell at different stages of its expansion which predict mm/sub-mm and far-IR emission line intensities from a series of key molecular and atomic constituents in the shell. The kinematic properties of the swept-up shell predicted by our model are in very good agreement with the measurements of the supershell detected in the nearby starburst galaxy M 82. We compare the modeling results with the ratio-ratio plots of the FIR/sub-mm/mm line emission in the central 1.0 kpc region to investigate the mechanism of star forming activity in M 82. Our model has yielded appropriate gas densities, temperatures, and structure scales compared to those measured in M 82, and the total H2 content is compatible with the observations. This implies that the neutral ISM of the central star-forming region is a product of fragments of the evolving shells.

arXiv commentApJ, accepted. 32 pages, 10 figures, 3 tables

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Cited by in corpus (7)

• A Census of the High-Density Molecular Gas in M82
• Tracing high density gas in M 82 and NGC 4038
• A High Resolution Map of 12CO J=6-5 Emission in the Starburst Galaxy M82
• CS Lines Profiles in Hot Cores
• Evolving Starburst Modeling of FIR/sub-mm/mm Line Emission. II. Application to M 82
• Environmental Dependence of Star Formation Law in the Disk and Center of IC 342
• Evolving Starburst Modeling of FIR/sub-mm/mm Line Emission. III. Application to Nearby Luminous Infrared Galaxies