By simulating the formation of disky galaxies, theorists have shown that gas from the intergalactic medium should be accreted along the plane of the galactic disk, while outflowing winds form cone-shaped structures centered about the rotation axis of the galaxy. It is predicted that, in the early universe, higher star formation rates should drive galactic winds to greater distance than is observed in the modern universe. Our study uses quasar spectra to probe at diffuse Mg II gas between redshift 0.65 and 1.6, and matched the resulting absorption lines with galaxies of the same redshift. Using Galfit, a galaxy modeling software, we have investigated the morphologies of these galaxies, and will be presenting our findings on the distribution of the galaxies’ azimuthal angles with respect to the quasar. We compare this distribution for galaxies that are and are not matched with Mg II absorption features. Although a small sample size limits our analysis, our results support a bimodal distribution of gas around disky galaxies and shows evidence of winds reaching distances as far as 120 kpc from their host galaxies.
