Monsters in Galactic Nuclei: Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies. I review the observed demographics and inferred evolution of supermassive black holes (BHs) found by dynamical modeling of spatially resolved kinematics. Most influential was the discovery of a tight correlation between BH mass and the velocity dispersion of the host-galaxy bulge. It and other correlations led to the belief that BHs and bulges coevolve by regulating each other's growth. New results are now replacing this simple story with a richer and more plausible picture in which BHs correlate differently with different galaxy components. BHs are found in pure-disk galaxies, so classical (elliptical-galaxy-like) bulges are not necessary to grow BHs. But BHs do not correlate with galaxy disks. And any correlations with disk-grown pseudobulges or halo dark matter are so weak as to imply no close coevolution. I suggest that there are four regimes of BH feedback. With these results, I suggest a picture of how star formation is quenched in galaxies, at least in the nearby universe. This talk is a summary of Kormendy & Ho 2013, ARA&A, 51, 511.
The Bishop Dinner will take place in the evening.