2012MNRAS.422..241A

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.