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IR Dust Bubbles II: Probing the Detailed Structure and Young Massive Stellar Populations of Galactic HII Regions

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arxiv 0901.1097 v1 pith:DNU2VMJG submitted 2009-01-08 astro-ph.GA

C. Watson , T. Corn , E.B. Churchwell , B.L. Babler , M.S. Povich , M.R. Meade , B.A. Whitney This is my paper · ORCID
classification astro-ph.GA
keywords bubblesidentifiedidentifydustemissionfittingsourcesstar-formation
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We present an analysis of late-O/early-B-powered, parsec-sized bubbles and associated star-formation using 2MASS, GLIMPSE, MIPSGAL and MAGPIS surveys. Three bubbles were selected from the Churchwell et al. (2007) catalog. We confirm that the structure identified in Watson et al. (2008) holds in less energetic bubbles, i.e. a PDR, identified by 8 um emission due to PAHs surrounds hot dust, identified by 24 um emission and ionized gas, identified by 20 cm continuum. We estimate the dynamical age of two bubbles by comparing bubble sizes to numerical models of Hosokawa & Inutsuka (2006). We also identify and analyze candidate young stellar objects (YSOs) using SED fitting and identify sites of possible triggered star-formation. Lastly, we identify likely ionizing sources for two sources based on SED fitting.

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  1. Bipolar HII regions Produced by Cloud-Cloud Collisions

    astro-ph.GA 2026-07 conditional novelty 5.0 of 10

    Head-on collisions of 500 M⊙ clouds form hub-filament systems and short-lived bipolar HII regions whose appearance depends strongly on viewing angle, with secondary radio and mid-IR metrics that may flag CCC origins.

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