The structure of HI in galactic disks: Simulations vs observations

Abstract

We generate synthetic Hi 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 Hi emission (in better agreement with observations) and more realistic spatial structure (including supernova blown bubbles). The synthetic data show Hi self-absorption with a morphology similar to that seen in observations. The density and temperature of the material responsible for Hi self-absorption is consistent with observationally determined values, and is found to be only weakly dependent on absorption strength and star formation efficiency.