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Davies et al. (2019) established that for L^* galaxies the fraction ofbaryons in the circumgalactic medium (CGM) is inversely correlated with themass of their central supermassive black holes (BHs) in the EAGLE hydrodynamicsimulation. The interpretation is that, over time, a more massive BH hasprovided more energy to transport baryons beyond the virial radius, whichadditionally reduces gas accretion and star formation. We continue thisresearch by focusing on the relationship between the 1) BH masses, 2) physicaland observational properties of the CGM, and 3) galaxy colours for MilkyWay-mass systems. The ratio of the cumulative BH feedback energy over thegaseous halo binding energy is a strong predictor of the CGM gas content, withBHs injecting >~10x the binding energy resulting in gas-poor haloes. Observabletracers of the CGM, including CIV, OVI, and HI absorption line measurements,are found to be effective tracers of the total z~0 CGM halo mass. We usehigh-cadence simulation outputs to demonstrate that BH feedback pushes baryonsbeyond the virial radius within 100 Myr timescales, but that CGM metal tracerstake longer (0.5-2.5 Gyr) to respond. Secular evolution of galaxies results inblue, star-forming or red, passive populations depending on the cumulativefeedback from BHs. The reddest quartile of galaxies with M_*=10^{10.2-10.7}M_solar (median u-r = 2.28) has a CGM mass that is 2.5x lower than the bluestquartile (u-r=1.59). We propose strategies for observing the predicted lowerCGM column densities and covering fractions around galaxies hosting moremassive BHs using the Cosmic Origins Spectrograph on Hubble.

Feedback from supermassive black holes transforms centrals into passive galaxies by ejecting circumgalactic gas