TY - JOUR
T1 - The blast view of the star-forming region in aquila (ℓ = 45°, b = 0°)
AU - Rivera-Ingraham, Alana
AU - Ade, Peter A.R.
AU - Bock, James J.
AU - Chapin, Edward L.
AU - Devlin, Mark J.
AU - Dicker, Simon R.
AU - Griffin, Matthew
AU - Gundersen, Joshua O.
AU - Halpern, Mark
AU - Hargrave, Peter C.
AU - Hughes, David H.
AU - Klein, Jeff
AU - Marsden, Gaelen
AU - Martin, Peter G.
AU - Mauskopf, Philip
AU - Netterfield, Calvin B.
AU - Olmi, Luca
AU - Patanchon, Guillaume
AU - Rex, Marie
AU - Scott, Douglas
AU - Semisch, Christopher
AU - Truch, Matthew D.P.
AU - Tucker, Carole
AU - Tucker, Gregory S.
AU - Viero, Marco P.
AU - Wiebe, Donald V.
PY - 2010/11/1
Y1 - 2010/11/1
N2 - 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 500μm 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 Hii 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 ∼103M⊙ for a dust emissivity index β = 1.5. The clump evolutionary stages range from evolved sources, with extended Hii regions and prominent IR stellar population, to massive young stellar objects, prior to the formation of an UCHiiR. The CORNISH datahave 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.
AB - 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 500μm 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 Hii 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 ∼103M⊙ for a dust emissivity index β = 1.5. The clump evolutionary stages range from evolved sources, with extended Hii regions and prominent IR stellar population, to massive young stellar objects, prior to the formation of an UCHiiR. The CORNISH datahave 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.
KW - Balloons - ISM
KW - Clouds - stars
KW - Color figures
KW - Formation - submillimeter
KW - ISM Online-only material
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U2 - 10.1088/0004-637X/723/1/915
DO - 10.1088/0004-637X/723/1/915
M3 - Article
AN - SCOPUS:78249280571
SN - 0004-637X
VL - 723
SP - 915
EP - 934
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
ER -