Volume 518, July-August 2010
Herschel: the first science highlights
|Number of page(s)||4|
|Published online||16 July 2010|
Letter to the Editor
Cold dust clumps in dynamically hot gas*
Astronomy & Space Science, Sejong University, 143-747, Seoul, South Korea e-mail: firstname.lastname@example.org
2 CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, 91191 Gif-sur-Yvette, France
3 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4 Center for Astrophysics, 60 Garden St., MS 67, Harvard University, Cambridge, MA 02138, USA
5 Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA
6 Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
7 314 Physics Building, Department of Physics and Astronomy, University of Missouri-Columbia, Columbia, MO 65211, USA
8 Department of Astronomy, Lab for Millimeter-wave Astronomy, University of Maryland, College Park, MD 20742-2421, USA
9 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
10 Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
11 Centre d'Étude Spatiale des Rayonnements, CNRS, 9 avenue du Colonel Roche, BP 4346, 31028 Toulouse, France
12 Observatoire Astronomique de Strasbourg, 11 rue de 1'université, 67000 Strasbourg, France
13 Center for Supercomputing and Astrophysics, Swinburne University of Technology, Hawthorn VIC 3122, Australia
14 CSIRO Australia Telescope National Facility, 76 Epping Rd., NSW1710, Australia
15 Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan
16 Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, Sakai, Osaka 599-8531, Japan
17 Spitzer Science Center, California Institute of Technology, MS 220-6, Pasadena, CA 91125, USA
18 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstra 85748 Garching, Germany
19 Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, Mail Stop 211-3, Moffett Field, CA 94035, USA
20 Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
Accepted: 16 April 2010
Aims. We present clumps of dust emission from Herschel observations of the Large Magellanic Cloud (LMC) and their physical and statistical properties. We catalog cloud features seen in the dust emission from Herschel observations of the LMC, the Magellanic type irregular galaxy closest to the Milky Way, and compare these features with H i catalogs from the ATCA+Parkes H i survey.
Methods. Using an automated cloud-finding algorithm, we identify clouds and clumps of dust emission and examine the cumulative mass distribution of the detected dust clouds. The mass of cold dust is determined from physical parameters that we derive by performing spectral energy distribution fits to 250, 350, and 500 μm emission from SPIRE observations using dust grain size distributions for graphite/silicate in low-metallicity extragalactic environments.
Results. The dust cloud mass spectrum follows a power law distribution with an exponent of γ = -1.8 for clumps larger than 4 × 102 and is similar to the H i mass distribution. This is expected from the theory of ISM structure in the vicinity of star formation.
Key words: submillimeter: ISM / Magellanic Clouds / ISM: structure / ISM: clouds
© ESO, 2010
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