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We analyze the properties of the circumgalactic gas (CGM) around 120 galaxieswith stellar and dark matter halo masses similar to that of the Milky Way. Wefocus on the morphology and kinematics of the neutral hydrogen and how thisdepends on f_g, the ratio of gas-to-stellar mass within the optical radius. Ingas-rich galaxies with f_g > 0.1, gas temperatures rise slowly from center ofthe halo out to the virial radius and average neutral gas column densitiesremain above 10^19 atoms cm^-2 out to radii of 50-70 kpc. In gas-poor galaxieswith f_g < 0.1, gas temperatures rise quickly outside the edge of the disk to10^6 K, and then remain fixed out to radii of 100 kpc. The column density ofneutral gas quickly drops below 10^19 atoms cm^-2 at radii of 10 kpc. Neutralgas distributions are also more asymmetric in gas-poor galaxies. Most of thedifferences between gas-poor and gas-rich galaxies in the Illustris simulationcan be attributed to the effects of "radio-mode" AGN feedback. In the Illustrissimulation, the circumgalactic gas is found to rotate coherently about thecenter of the galaxy with a maximum rotational velocity of around 200 km/s. Ingas-rich galaxies, the average coherence length of the rotating gas is 40 kpc,compared to 10 kpc in gas-poor galaxies. In the very most gas-rich systems, theCGM can rotate coherently over scales of 70-100 kpc. We discuss our results inthe context of recent observations of the CGM in low mass galaxies via UVabsorption-line spectroscopy and deep 21cm observations of edge-on spiralgalaxies.

The morphology and kinematics of neutral hydrogen in the vicinity of z=0 galaxies with Milky Way masses -- a study with the Illustris simulation