On the Origin of Exponential Galaxy Disks
  We use a disk galaxy evolution model to investigate whether galaxies with exponential surface brightness profiles can be produced in a cosmologically motivated framework for disk galaxy formation. Our model follows the accretion, cooling, and ejection of baryonic mass, as a function of radius, inside growing dark matter haloes. The surface density profile of the disk is determined by detailed angular momentum conservation, starting from the distribution of specific angular momentum as found in cosmological simulations. Exponential and quasi-exponential disks can be produced by our model through a combination of supernova driven galactic outflows (which preferentially remove low angular momentum material), intrinsic variation in the angular momentum distribution of the halo gas, and the inefficiency of star formation at large radii. We use observations from the SDSS NYU-VAGC to show that the median Sersic index of blue galaxies is a strong function of stellar mass. For blue galaxies, low mass galaxies have a median n=1.3, while high mass galaxies have a median n=4. Our model with energy driven outflows correctly reproduces this trend, whereas our models with momentum driven outflows and no outflows over predict the Sersic indices in low mass galaxies. We show that the observed fraction of "bulge-less" exponential galaxies is a strong function of stellar mass. For Milky-Way mass galaxies less than 0.1% of blue galaxies are bulge-less, whereas for M33 mass galaxies bulge-less and quasi-bulgeless galaxies are typical. These results suggest that the difficulty of hierarchical formation models to produce bulge-less Milky-Way mass galaxies is in fact not a problem. However, the problem of producing M33 like galaxies remains, and will provide a key test for hierarchical galaxy formation models. [Abridged] 
Aaron A. Dutton (UCO/Lick Observatory)