Conference paper Open Access
Physical processes that occur the circumgalactic medium (CGM) are largely responsible for setting the baryonic angular momentum of simulated galaxies. However, the angular momentum of the CGM has yet to be characterized in a large cosmological simulation, which are now capable of reproducing observed angular momentum properties for large populations of galaxies. We present a first step towards understanding the angular momentum properties of the CGM statistically for galaxies in the IllustrisTNG simulation. We focus on Milky Way-mass halos at $z=0$, but plan to extend this analysis to other masses and redshifts in future work.