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Interstellar Dust Models: Extinction, Absorption and Emission

Published online by Cambridge University Press:  26 February 2009

F. Boulanger ,
C. Joblin ,
A. Jones ,
S. Madden  and
B.T. Draine
B.T. Draine*
Affiliation:
Princeton University, Princeton NJ 08544-1001, USA
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Abstract

The observational constraints on interstellar dust are summarized. A dust model, consisting of a mixture of amorphous silicate, graphite, and PAH material that reproduces the observed interstellar extinction, is described. It is used to calculate the infrared emission expected when such dust is heated by radiation with the spectrum of interstellar starlight with various intensities. By adopting a suitable size distribution for the smallest carbonaceous grains (PAHs), and a distribution of starlight intensities, one can reproduce the observed global emission spectrum of galaxies. This allows the total dust mass, and the PAH abundance, to be estimated for any galaxy with a spectral energy distribution measured by the IRAC and MIPS cameras on Spitzer Space Telescope. For the Spitzer Infrared Nearby Galaxies Survey (SINGS) sample, galaxies with metallicities Z > 0.3 Z๏ tend to have a major fraction of their refractory elements in dust grains, just as in the Milky Way. For lower metallicity galaxies with extended H I envelopes, the overall dust-to-metals ratio remains uncertain. The PAH abundance index qPAH (the fraction of the total dust mass in PAH particles with NC < 103 C atoms) is dependent on metallicity: galaxies with Z <0.3 Z๏ have median qPAH = 1.1%, whereas galaxies with Z > 0.3 Z๏ have median qPAH = 3.5%. The reasons for the pronounced dependence of qPAH on metallicity remain unclear.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 35: Interstellar Dust from Astronomical Observations to Fundamental Studies , 2009 , pp. 245 - 268
Copyright
© EAS, EDP Sciences, 2009

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