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Published November 1, 2010 | Published
Journal Article Open

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


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 deg^2 (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 (UCH_(II)Rs) 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 ~10^3 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 UCH_(II)R. The CORNISH data have revealed the details of the stellar content and structure of the UCH_(II)Rs. 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.

Additional Information

© 2010 American Astronomical Society. Received 2010 May 27; accepted 2010 September 6; published 2010 October 15. The BLAST collaboration acknowledges the support of NASA through grants NAG5-12785, NAG5-13301, and NNGO- 6GI11G, the Canadian Space Agency (CSA), the UK Particle Physics and Astronomy Research Council (PPARC), the Canada Foundation for Innovation (CFI), the Ontario Innovation Trust (OIT), and Canada's Natural Sciences and Engineering Research Council (NSERC). We also thank the Columbia Scientific Balloon Facility (CSBF) staff for their outstanding work. We also thank the referee for very useful suggestions and improvements to our paper, and Mubdi Rahman for useful discussions.

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Published - RiveraIngraham2010p12054Astrophys_J.pdf


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