EDP Sciences
Press Release
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Free Access
Issue
A&A
Volume 504, Number 2, September III 2009
Page(s) 415 - 427
Section Galactic structure, stellar clusters, and populations
DOI https://doi.org/10.1051/0004-6361/200811568
Published online 13 May 2009
A&A 504, 415-427 (2009)
DOI: 10.1051/0004-6361/200811568

ATLASGAL – The APEX telescope large area survey of the galaxy at 870  $\mathsf{\mu}$m

F. Schuller1, K. M. Menten1, Y. Contreras1, 2, F. Wyrowski1, P. Schilke1, L. Bronfman2, T. Henning3, C. M. Walmsley4, H. Beuther3, S. Bontemps5, R. Cesaroni4, L. Deharveng6, G. Garay2, F. Herpin5, B. Lefloch7, H. Linz3, D. Mardones2, V. Minier8, S. Molinari9, F. Motte8, L.-Å. Nyman10, V. Reveret10, C. Risacher10, D. Russeil6, N. Schneider8, L. Testi11, T. Troost1, T. Vasyunina3, M. Wienen1, A. Zavagno6, A. Kovacs1, E. Kreysa1, G. Siringo1, and A. Weiß1

1  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
    e-mail: schuller@mpifr-bonn.mpg.de
2  Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
3  Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
4  Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
5  Laboratoire d'Astrophyisique de Bordeaux – UMR 5804, CNRS – Université Bordeaux 1, BP 89, 33270 Floirac, France
6  Laboratoire d'Astrophysique de Marseille – UMR 6110, CNRS – Université de Provence, 13388, Marseille Cedex 13, France
7  Laboratoire d'Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
8  Laboratoire AIM, CEA/IRFU – CNRS – Université Paris Diderot, Service d'Astrophysique, 91191 Gif-sur-Yvette, France
9  Istituto Fisica Spazio Interplanetario – INAF, via Fosso del Cavaliere 100, 00133 Roma, Italy
10  ESO, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
11  ESO, Karl Schwarzschild-Strasse 2, 85748 Garching bei München, Germany

Received 22 December 2008 / Accepted 20 February 2009

Abstract
Context. Thanks to its excellent 5100 m high site in Chajnantor, the Atacama Pathfinder Experiment (APEX) systematically explores the southern sky at submillimeter wavelengths, in both continuum and spectral line emission. Studying continuum emission from interstellar dust is essential to locating the highest density regions in the interstellar medium, and deriving their masses, column densities, density structures, and large-scale morphologies. In particular, the early stages of (massive) star formation remain poorly understood, mainly because only small samples of high-mass proto-stellar or young stellar objects have been studied in detail so far.
Aims. Our goal is to produce a large-scale, systematic database of massive pre- and proto-stellar clumps in the Galaxy, to understand how and under what conditions star formation takes place. Only a systematic survey of the Galactic Plane can provide the statistical basis for unbiased studies. A well characterized sample of Galactic star-forming sites will deliver an evolutionary sequence and a mass function of high-mass, star-forming clumps. This systematic survey at submillimeter wavelengths also represents a preparatory work for Herschel and ALMA.
Methods. The APEX telescope is ideally located to observe the inner Milky Way. The Large APEX Bolometer Camera (LABOCA) is a 295-element bolometer array observing at 870 $\mu$m, with a beam size of $19\farcs2$. Taking advantage of its large field of view (11$\farcm4$) and excellent sensitivity, we started an unbiased survey of the entire Galactic Plane accessible to APEX, with a typical noise level of 50-70 mJy/beam: the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL).
Results. As a first step, we covered ~95 deg2 of the Galactic Plane. These data reveal ~6000 compact sources brighter than 0.25 Jy, or 63 sources per square degree, 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 H II regions, or young embedded clusters, thus tracing more evolved stages after massive stars have formed. 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 $M_{\odot}$. In this first introductory paper, we show preliminary results from these ongoing observations, and discuss the mid- and long-term perspectives of the survey.


Key words: surveys -- submillimeter -- ISM: structure -- dust, extinction -- stars: formation -- Galaxy: disk



© ESO 2009

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