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Dust and pahs in low metallicity dwarf galaxies

Published online by Cambridge University Press:  04 October 2008

C. Kramer ,
S. Aalto ,
R. Simon  and
S.C. Madden
S.C. Madden*
Affiliation:
CEA Saclay, Service d'Astrophysique, France
*
smadden@cea.fr
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Abstract

Dwarf galaxies are currently enjoying wide popularity as more sensitive telescopes are able to unveil their dust emission properties in the mid-infrared to submillimetre wavelengths. Once thought to be an insignificant component of their ISM, the dust in dwarf galaxies can now be studied in greater detail with ISO and Spitzer and soon, Herschel, as well as new ground-based submillimetre telescopes. The mid-infrared to millimetre spectral energy distributions reveal global dust properties which look to be different from more metal-rich starburst galaxies, or our own Galaxy: a) deficit of PAHs; b) abundant very small grains; c) excess submillimetre emission that has been interpreted as very cold (<10 K) dust, thus containing up to 50% of the dust mass of the galaxies. The molecular clouds, and the morphology of the ISM appear to differ dramatically. These properties can be explained by the low metallicity environments and the young massive star formation activity, supernovae activity and chemical abundances.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 31: Far-Infrared Workshop 2007 , 2008 , pp. 123 - 128
Copyright
© EAS, EDP Sciences, 2008

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