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The ISM of Low Metallicity Galaxies: The Herschel view

Published online by Cambridge University Press:  21 March 2013

Suzanne C. Madden ,
Aurélie Rémy ,
Frédéric Galliano ,
Maud Galametz ,
George Bendo ,
Diane Cormier ,
Vianney Lebouteiller ,
Sacha Hony  and
Herschel SAG 2 consortium
Suzanne C. Madden
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
Aurélie Rémy
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
Frédéric Galliano
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
Maud Galametz
Affiliation:
Institute of Astronomy, University of Cambridge, Madingly Rd., Cambridge, UK
George Bendo
Affiliation:
Alma Regional Center, University of Manchester, Oxford Rd., Machester, UK
Diane Cormier
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
Vianney Lebouteiller
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
Sacha Hony
Affiliation:
CEA Saclay, DSM, AIM, Service d'Astrophysique, Gif-sur-Yvette 91911, France, email: [email protected]
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Abstract

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The wide variety of low metallicity galaxies of the local universe serve as convenient laboratories to study the evolution of gas and dust and conditions for star formation in environments which may resemble those of the early universe. The Herschel Dwarf Galaxy Survey is studying the far infrared (FIR) and submillimeter (submm) properties of the gas and dust in galaxies with metallicity values as low as 1/45 that of solar. With complementary Spitzer, Laboca/APEX, Scuba/JCMT data, the dust spectral energy distributions are well constrained now, providing more accurate dust masses. We find a steep drop in dust-to-gas mass ratio (D/G) when the metallicity is below 12+log(O/H) ∼ 8. A submillimeter excess can be found in some low metallicity galaxies, which, when present, becomes apparent at wavelengths at or longer than 500 μm. While CO is difficult to observe in low metallicity gas, the FIR fine structure lines, on the other hand, are very luminous and highlight a potentially important reservoir of CO-free molecular gas, better traced by the 158 μm [CII] line.

Keywords

galaxies: dwarf — galaxies: ISM — ISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 127 - 134
Copyright
Copyright © International Astronomical Union 2013

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