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ATLASGAL - The APEX Telescope Large Area Survey of the Galaxy at 870 microns | F. Schuller
; K.M. Menten
; Y. Contreras
; F. Wyrowski
; P. Schilke
; L. Bronfman
; T. Henning
; C.M. Walmsley
; H. Beuther
; S. Bontemps
; R. Cesaroni
; L. Deharveng
; G. Garay
; F. Herpin
; B. Lefloch
; H. Linz
; D. Mardones
; V. Minier
; S. Molinari
; F. Motte
; L.-A. Nyman
; V. Reveret
; C. Risacher
; D. Russeil
; N. Schneider
; L. Testi
; T. Troost
; T. Vasyunina
; M. Wienen
; A. Zavagno
; A. Kovacs
; E. Kreysa
; G. Siringo
; A. Weiss
; | Date: |
7 Mar 2009 | Abstract: | (Abridged) Studying continuum emission from interstellar dust is essential to
locate and characterize the highest density regions in the interstellar medium.
In particular, the early stages of massive star formation are still mysterious.
Our goal is to produce a large scale, systematic database of massive pre- and
proto-stellar clumps in the Galaxy, in order to better understand how and under
what conditions star formation takes place. A well characterized sample of
star-forming sites will deliver an evolutionary sequence and a mass function of
high-mass star-forming clumps. Such a systematic survey at submm wavelengths
also represents a pioneering work in preparation for Herschel and ALMA. The
APEX telescope is ideally located to observe the inner Milky Way. The recently
commissioned Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer
array observing at 870 microns, with a beam of 19". Taking advantage of its
large field of view (11.4’) and excellent sensitivity, we have started an
unbiased survey of the Galactic Plane, with a noise level of 50-70 mJy/beam:
the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL). As a first step,
we have covered 95 sq. deg. These data reveal 6000 compact sources brighter
than 0.25 Jy, as well as extended structures, many of them filamentary. About
two thirds of the compact sources have no bright infrared counterpart, and some
of them are likely to correspond to the precursors of (high-mass) proto-stars
or proto-clusters. Other compact sources harbor hot cores, compact HII regions
or young embedded clusters. Assuming a typical distance of 5 kpc, most sources
are clumps smaller than 1 pc with masses from a few 10 to a few 100 M_sun. In
this introductory paper, we show preliminary results from these ongoing
observations, and discuss the perspectives of the survey. | Source: | arXiv, 0903.1369 | Services: | Forum | Review | PDF | Favorites |
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