THE BLAST VIEW OF THE STAR-FORMING REGION IN AQUILA (ℓ = 45°,b= 0°)

Abstract

We have carried out the first general submillimeter analysis of the field towards 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 COR-NISH 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 (IRDCs). 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 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.

Trigonometric parallaxes of star-forming regions in the Sagittarius spiral arm

“…A.1.13. G045.07+00.13 G045.07+00.13 hosts numerous ultra-compact H II regions, maser sources, and outflows from young and highly embedded OB stellar clusters (Rivera-Ingraham et al 2010). The V LS R is 59 km s −1 (from the 13CO GRS survey).…”

HERSCHELOBSERVATIONS OF THE W3 GMC: CLUES TO THE FORMATION OF CLUSTERS OF HIGH-MASS STARS

“…W3 East is the most active of the two in terms of the associated (external and internal) stellar population. Using the technique of Rivera-Ingraham et al (2010) we estimate that the luminosity of the W3 East clump is equivalent to a single-star ZAMS spectral type (Panagia 1973) of ∼O7. However, because we did not use the 70 µm datum in fitting the SED, the temperature and luminosity of this hot source are poorly constrained, and so the allowed range of spectral type is wide, B0.5 to O6.…”

THE BALLOON-BORNE LARGE APERTURE SUBMILLIMETER TELESCOPE (BLAST) 2005: A 10 deg2SURVEY OF STAR FORMATION IN CYGNUS X

“…For sufficiently massive stars, significant ionization of the surroundings will ensue, producing a hypercompact H ii region. There could be many within a single clump, for example (Rivera-Ingraham et al 2010). These clumps would appear in the L-M diagram near the empirical nuclear burning locus (see Section 5.4).…”