Why do galaxies stop forming stars? I. The passive fraction - black hole
  mass relation for central galaxies
  We derive the dependence of the fraction of passive central galaxies on the
mass of their supermassive black holes for a sample of over 400,000 SDSS
galaxies at z < 0.2. Our large sample contains galaxies in a wide range of
environments, with stellar masses 8 < log(M*/Msun) < 12, spanning the entire
morphological spectrum from pure disks to spheroids. We derive estimates for
the black hole masses from measured central velocity dispersions and bulge
masses, using a variety of published empirical relationships. We find a very
strong dependence of the passive fraction on black hole mass, which is largely
unaffected by the details of the black hole mass estimate. Moreover, the
passive fraction relationship with black hole mass remains strong and tight
even at fixed values of galaxy stellar mass (M*), dark matter halo mass
(Mhalo), and bulge-to-total stellar mass ratio (B/T). Whereas, the passive
fraction dependence on M*, Mhalo and B/T is weak at fixed MBH. These
observations show that, for central galaxies, MBH is the strongest correlator
with the passive fraction, consistent with quenching from AGN feedback.
