The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 square degree Galactic Plane Survey in Vulpecula (l=59°) .

Details The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 square degree Galactic Plane Survey in Vulpecula (l=59°) . The Balloon-borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 square degree Galactic Plane Survey in Vulpecula (l=59°) .

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111606r&link_type=abstract

American Astronomical Society, AAS Meeting #211, #116.06; Bulletin of the American Astronomical Society, Vol. 39, p.945

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We present the first results from a new 250, 350 and 500 micron Galactic plane survey taken with the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST) in 2005. This survey's primary goal is to identify and characterize high-mass proto-stellar objects. The region studied here covers 4 square degrees near the open cluster NGC 6823 in the constellation Vulpecula (l=59°). We find 60 compact sources (< 60" diameter) detected simultaneously in all three bands. Their spectral energy distributions are constrained through BLAST, IRAS, Spitzer MIPS and MSX photometry, with inferred dust temperatures spanning 12-40 K assuming a dust emissivity index beta=1.5. The luminosity-to-mass ratio, a distance-independent quantity, spans 0.2-130 solar luminosities/solar mass. Distances are estimated from coincident 13CO velocities combined with a variety of other velocity and morphological data in the literature. In total, 49 sources are associated with a molecular cloud complex encompassing NGC 6823 (distance 2.3 kpc), 10 objects with the Perseus Arm (distance 8.5 kpc) and one object is probably in the outer Galaxy (distance 14 kpc). Near NGC 6823, the inferred luminosities and masses of BLAST sources span 40-10000 solar luminosities, and 15-700 solar masses respectively. The mass spectrum is compatible with molecular gas masses in other high-mass star forming regions. Several luminous sources appear to be Ultra Compact HII regions powered by early B stars. However, most of the objects are cool, massive gravitationally-bound clumps with no obvious internal radiation from a protostar.

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