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We derive the dependence of the fraction of passive central galaxies on themass of their supermassive black holes for a sample of over 400,000 SDSSgalaxies at z < 0.2. Our large sample contains galaxies in a wide range ofenvironments, with stellar masses 8 < log(M*/Msun) < 12, spanning the entiremorphological spectrum from pure disks to spheroids. We derive estimates forthe black hole masses from measured central velocity dispersions and bulgemasses, using a variety of published empirical relationships. We find a verystrong dependence of the passive fraction on black hole mass, which is largelyunaffected by the details of the black hole mass estimate. Moreover, thepassive fraction relationship with black hole mass remains strong and tighteven at fixed values of galaxy stellar mass (M*), dark matter halo mass(Mhalo), and bulge-to-total stellar mass ratio (B/T). Whereas, the passivefraction dependence on M*, Mhalo and B/T is weak at fixed MBH. Theseobservations show that, for central galaxies, MBH is the strongest correlatorwith the passive fraction, consistent with quenching from AGN feedback.

Why do galaxies stop forming stars? I. The passive fraction - black hole mass relation for central galaxies