The cool, 1e4K, phase of the circumgalactic medium, is predicted by classical models to be relatively short lived, accreting onto the galaxy within the halo dynamical time and fueling star formation. Observations, on the other hand, show this gas is ubiquitous, with high detection rates around both star-forming and quiescent galaxies, revealing a gap in our understanding of the galactic baryon cycle, CGM physics, or both. I will present recent work addressing the properties of the cool CGM across halo and galaxy mass at low redshifts. We construct phenomenological models and apply them to observations to constrain the gas mass, thermal properties, and its morphology. We find that the cool CGM mass may constitute a constant fraction of the halo baryon budget across 3 orders of magnitude in halo mass, and be supported by non-thermal mechanisms. We examine the CGM accretion rates onto the galaxy, compare them to the galactic star formation rates, and explore mechanisms which may slow or prevent this accretion.
