Статья

The Balloon‐borne Large Aperture Submillimeter Telescope (BLAST) 2005: A 4 deg<sup>2</sup>Galactic Plane Survey in Vulpecula (ℓ = 59°)

Edward L. ChapinDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaP. A. R. AdeDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UKJ. J. BockJet Propulsion Laboratory, Pasadena, CA 91109-8099C. M. BruntSchool of Physics, University of Exeter, Exeter EX4 4QL, UKMichelle DevlinDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104Simon DickerDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104M. GriffinDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UKJoshua O. GundersenDepartment of Physics, University of Miami, Carol Gables, FL 33146M. HalpernDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaPeter HargraveDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UKDavid H. HughesInstituto Nacional de Astrofísica Óptica y Electrónica (INAOE), 72000 Puebla, MexicoJeff KleinDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104G. MarsdenDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaP. G. MartinCanadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON M5S 3H8, CanadaP. MauskopfDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UKC. B. NetterfieldDepartment of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, CanadaL. OlmiIstituto di Radioastronomia, I-50125 Florence, ItalyE. PascaleDepartment of Physics, University of Toronto, Toronto, ON M5S 1A7, CanadaG. PatanchonDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaM. RexDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104D. ScottDepartment of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T 1Z1, CanadaChristopher SemischDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104Matthew D. P. TruchDepartment of Physics, Brown University, Providence, RI 02912C. TuckerDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3AA, UKGregory S. TuckerDepartment of Physics, Brown University, Providence, RI 02912M. VieroDepartment of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H4, CanadaDonald WiebeDepartment of Physics, University of Toronto, Toronto, ON M5S 1A7, Canada

2008en

ABI

Аннотация

We present the first results from a new 250, 350, and 500 μm 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 protostellar objects (HMPOs). The region studied here covers 4 deg^2 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 SEDs are constrained through BLAST, IRAS, Spitzer MIPS, and MSX photometry, with inferred dust temperatures spanning ~12-40 K assuming a dust emissivity index β = 1.5. The luminosity-to-mass ratio, a distance-independent quantity, spans ~0.2-130 L_☉ M^(−1)_☉. Distances are estimated from coincident ^(13)CO(1→ 0) 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 (~8.5 kpc), and one object is probably in the outer Galaxy (~14 kpc). Near NGC 6823, the inferred luminosities and masses of BLAST sources span ~40-10^4 L_☉ and ~15-700 M_☉, respectively. The mass spectrum is compatible with molecular gas masses in other high-mass star-forming regions. Several luminous sources appear to be ultracompact H II regions powered by early B stars. However, many of the objects are cool, massive gravitationally bound clumps with no obvious internal radiation from a protostar, and hence excellent HMPO candidates.

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Идентификаторы

DOI: 10.1086/588544

Цитирования и источники

Цитирований: 2Использованных источников: 0

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