The BLAST view of the star-forming region in aquila (ℓ= 45°,b= 0°)

Rivera-Ingraham, Alana, Ade, Peter A. R. ORCID: https://orcid.org/0000-0002-5127-0401, Bock, James J., Chapin, Edward L., Devlin, Mark J., Dicker, Simon R., Griffin, Matthew Joseph ORCID: https://orcid.org/0000-0002-0033-177X, Gundersen, Joshua O., Halpern, Mark, Hargrave, Peter Charles ORCID: https://orcid.org/0000-0002-3109-6629, Hughes, David H., Klein, Jeff, Marsden, Gaelen, Martin, Peter G., Mauskopf, Philip Daniel ORCID: https://orcid.org/0000-0001-6397-5516, Netterfield, Calvin B., Olmi, Luca, Patanchon, Guillaume, Rex, Marie, Scott, Douglas, Semisch, Christopher, Truch, Matthew D. P., Tucker, Carole Elizabeth ORCID: https://orcid.org/0000-0002-1851-3918, Tucker, Gregory S., Viero, Marco P. and Wiebe, Donald V. 2010. The BLAST view of the star-forming region in aquila (ℓ= 45°,b= 0°). Astrophysical Journal 723 (1) , pp. 915-934. 10.1088/0004-637X/723/1/915

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Abstract

We have carried out the first general submillimeter analysis of the field toward GRSMC 45.46+0.05, a massive star-forming region in Aquila. The deconvolved 6 deg2 (3° × 2°) maps provided by BLAST in 2005 at 250, 350, and 500 μm were used to perform a preliminary characterization of the clump population previously investigated in the infrared, radio, and molecular maps. Interferometric CORNISH data at 4.8 GHz have also been used to characterize the Ultracompact H II regions (UCHIIRs) within the main clumps. By means of the BLAST maps, we have produced an initial census of the submillimeter structures that will be observed by Herschel, several of which are known Infrared Dark Clouds. Our spectral energy distributions of the main clumps in the field, located at ~7 kpc, reveal an active population with temperatures of T~ 35-40 K and masses of ~103 M for a dust emissivity index β = 1.5. The clump evolutionary stages range from evolved sources, with extended H II regions and prominent IR stellar population, to massive young stellar objects, prior to the formation of an UCHIIR. The CORNISH data have revealed the details of the stellar content and structure of the UCHIIRs. In most cases, the ionizing stars corresponding to the brightest radio detections are capable of accounting for the clump bolometric luminosity, in most cases powered by embedded OB stellar clusters.

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Physics and Astronomy
Subjects:	Q Science > QB Astronomy
Uncontrolled Keywords:	Balloons ; ISM: clouds; Stars: formation ; Submillimeter: ISM
Publisher:	American Astronomical Society
ISSN:	0004-637X
Last Modified:	18 Oct 2022 12:44
URI:	https://orca.cardiff.ac.uk/id/eprint/11024

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