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Molecules as tracers of galaxy evolution

Published online by Cambridge University Press:  21 March 2013

Susanne Aalto
Susanne Aalto*
Affiliation:
Department of Earth and Space Sciences, Chalmers University of Technology Onsala Space Observatory, SE-439 92 Onsala, Sweden email: saalto@chalmers.se
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Abstract

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Studying the molecular phase of the interstellar medium in galaxies is fundamental for the understanding of the onset and evolution of star formation and the growth of supermassive black holes. We can use molecules as observational tools exploiting them as tracers of chemical, physical and dynamical conditions. In this short review, key molecules (e.g. HCN, HCO+, HNC, HC3N, CN, H3O+) in identifying the nature of buried activity and its evolution are discussed including some standard astrochemical scenarios. Furthermore, we can use IR excited molecular emission to probe the very inner regions of luminous infrared galaxies (LIRGs) allowing us to get past the optically thick dust barrier of the compact obscured nuclei, e.g. in the dusty LIRG NGC4418. High resolution studies are often necessary to separate effects of excitation and radiative transport from those of chemistry - one example is absorption and effects of stimulated emission in the ULIRG Arp220. Finally, molecular gas in large scale galactic outflows is briefly discussed.

Keywords

galaxies: evolution — galaxies: ISM — galaxies: active — radio lines: ISM — ISM: molecules — ISM: abundances — astrochemistry
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. 199 - 208
Copyright
Copyright © International Astronomical Union 2013

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