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The structure of H i in galactic discs: simulations versus observations




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.

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