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Using our measurements of the H$\alpha$ emission line flux originating in thecool (T $\sim10^4$ K) gas that populates the halos of galaxies, we build ajoint model to describe mass of the cool circumgalactic medium (CGM) as afunction of galactic stellar mass ($10^{9.5} < ({\rm M_*/M}_\odot) < 10^{11}$)and environment. Because the H$\alpha$ emission correlates with the maincooling channel for this gas, we are able to estimate the rate at which the CGMcools and becomes fuel for star formation in the central galaxy. We describethis calculation, which uses our observations, previous measurements of somecritical CGM properties, and modeling of the cooling mechanism using the\cloudy modeling suite. We find that the mass cooling rate is larger than thestar formation rates of the central galaxies by a factor of $\sim 4 - 90$,empirically confirming that there is sufficient fuel to resolve the gasconsumption problem and that feedback is needed to avoid collecting too muchcold gas in galaxies. We find excellent agreement between our estimates of boththe mass cooling rates and mass loading factors and the predictions ofindependent theoretical studies. The convergence in results that we find fromseveral completely different treatments of the problem, particularly at thelower end of the galactic mass range, is a strong indication that we have arelatively robust understanding of the quantitative effects of feedback acrossthis mass range.

An Empirical Determination of the Dependence of the Circumgalactic Mass Cooling Rate and Feedback Mass Loading Factor on Galactic Stellar Mass