Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545914h&link_type=abstract
American Astronomical Society, AAS Meeting #215, #459.14; Bulletin of the American Astronomical Society, Vol. 42, p.487
Astronomy and Astrophysics
Astronomy
Scientific paper
We present a study into the properties of the dust and complex molecules in and around selected HII regions in the Large Magellanic Cloud. The analysis is based on the Spitzer program SAGE (Surveying the Agents of a Galaxy's Evolution). Because of the lower metallicity environment, dust shielding is reduced and the effects of the ultraviolet radiation carry further than in the Milky way. Because of this these HII regions may better represent star forming regions in the more distant universe.
We present the near- to far-IR spectral energy distributions (SEDs) as a function of radial distance to the center of the several clusters. The regions span a wide range in luminosities. We have developed a self consistent spherical clumpy dust radiative transfer model to interpret the observed trends. The model treats the detailed dust optical properties and transient grain heating as well as IR absorption and reprocession. This allows us to interpret the observed variations in SED in terms of the clumpiness, varying incident radiation-field and changing abundances of polycyclic aromatic hydrocarbons (PAHs), transiently heated very small grains (VSG) to submicron-sized grains in thermal equilibrium, i.e. in terms of the varying grain-size distribution.
We find that the LMC massive star forming sites are typified by a several parsec sized void and clumpiness and PAH abundance which increases with distance from the central illuminating source. The inner void may be the result of massive star winds. The observed flat mid-IR SEDs require a grain-size distribution skewed to a higher fraction of smaller grains compared to the Milky Way dust.
Galliano Frederic
Hony Sacha
Madden S. M.
SAGE Consortium
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