Journal Article

The structure of H <span class="smallCaps">i</span> in galactic discs: simulations versus observations

David M. Acreman, Clare L. Dobbs, Christopher M. Brunt and Kevin A. Douglas

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 422, issue 1, pages 241-251
Published in print May 2012 | ISSN: 0035-8711
Published online April 2012 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2012.20599.x
The structure of H i in galactic discs: simulations versus observations

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We generate synthetic H i Galactic plane surveys from spiral galaxy simulations which include stellar feedback processes. Compared to a model without feedback we find an increased scale height of H i emission (in better agreement with real observations) and more realistic spatial structure (including supernova blown bubbles). The synthetic data show H i self-absorption with a morphology similar to that seen in observations. The density and temperature of the material responsible for H i self-absorption is consistent with observationally determined values, and is found to be only weakly dependent on absorption strength and star formation efficiency.

Keywords: methods: numerical; surveys; ISM: atoms; ISM: structure

Journal Article.  6290 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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