Volume 518, July-August 2010
Herschel: the first science highlights
|Number of page(s)||5|
|Published online||16 July 2010|
Letter to the Editor
Determining dust temperatures and masses in the Herschel era: The importance of observations longward of 200 micron*
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: email@example.com
2 CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, 91191 Gif-sur-Yvette, France
3 Centre d'Étude Spatiale des Rayonnements, CNRS, 9 av. du Colonel Roche, BP 4346, 31028 Toulouse, France
4 Department of Astronomy, University of Maryland. College Park, MD 20742, USA
5 Observatoire Astronomique de Strasbourg, 11 rue de l'université, 67000 STRASBOURG, France
6 Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA
7 Centre for Supercomputing and Astrophysics, Swinburne University of Technology, Hawthorn VIC 3122, Australia
8 CSIRO Australia Telescope National Facility, PO Box 76, Epping NSW 1710, Australia
9 Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
10 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics & Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK
11 Astronomy & Space Science, Sejong University, 143-747, Seoul, South Korea
12 314 Physics Building, Department of Physics and Astronomy, University of Missouri, Columbia, MO 65211, USA
13 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
14 MSSL, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
15 Visiting Scientist at Smithsonian Astrophysical Observatory, Harvard-CfA, 60 Garden St., Cambridge, MA, 02138, USA
16 Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago, Chile
17 Spitzer Science Center, California Institute of Technology, MS 220-6, Pasadena, CA 91125, USA
18 Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, Mail Stop 211-3, Moffett Field, CA 94035, USA
Accepted: 1 May 2010
Context. The properties of the dust grains (e.g., temperature and mass) can be derived from fitting far-IR SEDs (≥100 μm). Only with SPIRE on Herschel has it been possible to get high spatial resolution at 200 to 500 μm that is beyond the peak (~160 μm) of dust emission in most galaxies.
Aims. We investigate the differences in the fitted dust temperatures and masses determined using only <200 μm data and then also including >200 μm data (new SPIRE observations) to determine how important having >200 μm data is for deriving these dust properties.
Methods. We fit the 100 to 350 μm observations of the Large Magellanic Cloud (LMC) point-by-point with a model that consists of a single temperature and fixed emissivity law. The data used are existing observations at 100 and 160 μm (from IRAS and Spitzer) and new SPIRE observations of 1/4 of the LMC observed for the HERITAGE key project as part of the Herschel science demonstration phase.
Results. The dust temperatures and masses computed using only 100 and 160 μm data can differ by up to 10% and 36%, respectively, from those that also include the SPIRE 250 & 350 μm data. We find that an emissivity law proportional to λ-1.5 minimizes the 100–350 μm fractional residuals. We find that the emission at 500 μm is ~10% higher than expected from extrapolating the fits made at shorter wavelengths. We find the fractional 500 μm excess is weakly anti-correlated with MIPS 24 μm flux and the total gas surface density. This argues against a flux calibration error as the origin of the 500 μm excess. Our results do not allow us to distinguish between a systematic variation in the wavelength dependent emissivity law or a population of very cold dust only detectable at λ ≥ 500 μm for the origin of the 500 μm excess.
Key words: ISM: general / galaxies: individual: LMC / Magellanic Clouds / infrared: ISM
© ESO, 2010
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