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

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