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We present an analysis of the role of feedback in shaping the neutralhydrogen (HI) content of simulated disc galaxies. For our analysis, we haveused two realisations of two separate Milky Way-like (~L*) discs - oneemploying a conservative feedback scheme (MUGS), the other significantly moreenergetic (MaGICC). To quantify the impact of these schemes, we generate zerothmoment (surface density) maps of the inferred HI distribution; construct powerspectra associated with the underlying structure of the simulated cold ISM, inaddition to their radial surface density and velocity dispersion profiles. Ourresults are compared with a parallel, self-consistent, analysis of empiricaldata from THINGS (The HI Nearby Galaxy Survey). Single power-law fits(P~k^gamma) to the power spectra of the stronger-feedback (MaGICC) runs (overspatial scales corresponding to 0.5 kpc to 20 kpc) result in slopes consistentwith those seen in the THINGS sample (gamma = -2.5). The weaker-feedback (MUGS)runs exhibit shallower power law slopes (gamma = -1.2). The power spectra ofthe MaGICC simulations are more consistent though with a two-component fit,with a flatter distribution of power on larger scales (i.e., gamma = -1.4 forscales in excess of 2 kpc) and a steeper slope on scales below 1 kpc (gamma =-5), qualitatively consistent with empirical claims, as well as our earlierwork on dwarf discs. The radial HI surface density profiles of the MaGICC discsshow a clear exponential behaviour, while those of the MUGS suite areessentially flat; both behaviours are encountered in nature, although theTHINGS sample is more consistent with our stronger (MaGICC) feedback runs.

The Role of Feedback in Shaping the Structure of the Interstellar Medium