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How does metallicity affect the gas and dust properties of galaxies?

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

Suzanne C. Madden ,
Diane Cormier  and
Aurélie Rémy-Ruyer
Suzanne C. Madden
Affiliation:
CEA/DSM/IRFU/Service d'Astrophysique, AIM (UMR 7158), 91191, Gif-sur-Yvette, France email: [email protected]
Diane Cormier
Affiliation:
Institute for Theoretical Astrophysics, Center for Astronomy, University of Heidelberg, 69120, Heidelberg, Germany email: [email protected]
Aurélie Rémy-Ruyer
Affiliation:
CEA/DSM/IRFU/Service d'Astrophysique, AIM (UMR 7158), 91191, Gif-sur-Yvette, France email: [email protected] Institut d'Astrophysique Spatiale, CNRS, 91405, Orsay, France email: [email protected]
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Abstract

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Comparison of the ISM properties of a wide range of metal poor galaxies with normal metal-rich galaxies reveals striking differences. We find that the combination of the low dust abundance and the active star formation results in a very porous ISM filled with hard photons, heating the dust in dwarf galaxies to overall higher temperatures than their metal-rich counterparts. This results in photodissociation of molecular clouds to greater depths, leaving relatively large PDR envelopes and difficult-to-detect CO cores. From detailed modeling of the low-metallicity ISM, we find significant fractions of CO-dark H2 - a reservoir of molecular gas not traced by CO, but present in the [CII] and [CI]-emitting envelopes. Self-consistent analyses of the neutral and ionized gas diagnostics along with the dust SED is the necessary way forward in uncovering the multiphase structure of galaxies.

Keywords

galaxies: dwarfgalaxies: ISMgalaxies: starburstinfrared: galaxies
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , pp. 191 - 198
Copyright
Copyright © International Astronomical Union 2016 

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