Abstract
The state of the interstellar medium (ISM) of dwarf galaxies is reviewed, thereby emphasizing three different phases, namely the neutral, the hot and the nonthermal ISM. The distribution and structure of the more diffuse neutral ISM is discussed mainly on the basis of observations of the neutral hydrogen (HI), while that of the dense gas relies mostly on observations of the carbon monoxide (CO) line. Relations between the gas surface density and the star formation density are discussed, with ionized carbon (CII) identified as a powerful future tracer of the dense gas phase in star-forming galaxies. The hot X-ray-emitting gas is interpreted in terms of galactic winds driven by star formation and subsequent supernovae, making dwarf galaxies plausible candidates for the metal enrichment of the intra-cluster medium (ICM) in the early universe. The nonthermal phase of the ISM, comprising relativistic particles and magnetic fields is reviewed in the light of the possible role of dwarf galaxies in the magnetization of the ICM in the early universe, competing here with AGN. With LOFAR, a new low-frequency facility is becoming operational which will greatly aid to disclose the relativistic phase of the ISM also in dwarf galaxies.
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Acknowledgements
I wish to thank the organizers of the meeting on dwarf galaxies, foremost Polychronis Papaderos, for the kind invitation to a very inspiring meeting. Part of my research on dwarf galaxies is supported by the Deutsche Forschungsgemeinschaft, via Grants KL 533/11-1 and FOR 1254/1.
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Klein, U. (2012). The ISM of Dwarf Galaxies. In: Papaderos, P., Recchi, S., Hensler, G. (eds) Dwarf Galaxies: Keys to Galaxy Formation and Evolution. Astrophysics and Space Science Proceedings. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-22018-0_2
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