Spatial Variations of Dust Abundances Across the Large Magellanic Cloud
Creators
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1.
Infrared Processing and Analysis Center
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2.
French National Centre for Scientific Research
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3.
University of Arizona
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4.
Harvard-Smithsonian Center for Astrophysics
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5.
University of Virginia
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6.
Nagoya University
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7.
University of Wisconsin–Madison
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8.
Space Telescope Science Institute
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9.
University of Toledo
Abstract
Using the data obtained with the Spitzer Space Telescope as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) legacy survey, we have studied the variations of the dust composition and abundance across the Large Magellanic Cloud (LMC). Such variations are expected, as the explosive events which have lead to the formation of the many H I shells observed should have affected the dust properties. Using a model and comparing with a reference spectral energy distribution from our Galaxy, we deduce the relative abundance variations of small dust grains across the LMC. We examined the infrared color ratios as well as the relative abundances of very small grains (VSGs) and polycyclic aromatic hydrocarbons (PAHs) relative to the big grain abundance. Results show that each dust component could have different origins or evolution in the interstellar medium (ISM). The VSG abundance traces the star formation activity and could result from shattering of larger grains, whereas the PAH abundance increases around molecular clouds as well as in the stellar bar, where they could have been injected into the ISM during mass loss from old stars.
Additional Information
© 2009 The American Astronomical Society. Received 2009 February 13; accepted 2009 April 28; published 2009 June 1.Attached Files
Published - Paradis2009p4611Astron_J.pdf
Files
Paradis2009p4611Astron_J.pdf
Additional details
Identifiers
- Eprint ID
- 15772
- Resolver ID
- CaltechAUTHORS:20090911-094407161
Dates
- Created
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2009-09-15Created from EPrint's datestamp field
- Updated
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2021-11-08Created from EPrint's last_modified field