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Title: DUST EMISSION FROM EVOLVED AND UNEVOLVED H II REGIONS IN THE LARGE MAGELLANIC CLOUD

Journal Article · · Astrophysical Journal
;  [1];  [2]; ;  [3];  [4]; ; ;  [5];  [6];  [7]
  1. Astronomy Department, University of Michigan, Ann Arbor, MI 48109 (United States)
  2. Department of Physics and Astronomy, University of Missouri, Columbia, MO 65211 (United States)
  3. Universit de Toulouse, UPS-OMP, IRAP, Toulouse (France)
  4. Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, WI 53706 (United States)
  5. Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
  6. Department of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903 (United States)
  7. Universities Space Research Association, Stratospheric Observatory for Infrared Astronomy, NASA Ames Research Center, MS 211-3, Moffett Field, CA 94035 (United States)

We present a study of the dust properties of 12 classical and superbubble H II regions in the Large Magellanic Cloud. We use infrared photometry from Spitzer (8, 24, 70, and 160 {mu} m bands), obtained as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) program, along with archival spectroscopic classifications of the ionizing stars to examine the role of stellar sources on dust heating and processing. Our infrared observations show surprisingly little correlation between the emission properties of the dust and the effective temperatures or bolometric magnitudes of stars in the H II regions, suggesting that the H II region evolutionary timescale is not on the order of the dust processing timescale. We find that the infrared emission of superbubbles and classical H II regions shows little differentiation between the two classes, despite the significant differences in age and morphology. We do detect a correlation of the 24 {mu} m emission from hot dust with the ratio of 70-160 {mu} m flux. This correlation can be modeled as a trend in the temperature of a minority hot dust component, while a majority of the dust remains significantly cooler.

OSTI ID:
21576866
Journal Information:
Astrophysical Journal, Vol. 732, Issue 2; Other Information: DOI: 10.1088/0004-637X/732/2/98; ISSN 0004-637X
Country of Publication:
United States
Language:
English