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We study the population of supermassive black holes (SMBHs) and their effectson massive central galaxies in the IllustrisTNG cosmological hydrodynamicalsimulations of galaxy formation. The employed model for SMBH growth andfeedback assumes a two-mode scenario in which the feedback from active galacticnuclei occurs through a kinetic, comparatively efficient mode at low accretionrates relative to the Eddington limit, and in the form of a thermal, lessefficient mode at high accretion rates. We show that the quenching of massivecentral galaxies happens coincidently with kinetic-mode feedback, consistentwith the notion that active supermassive black cause the low specific starformation rates observed in massive galaxies. However, major galaxy mergers arenot responsible for initiating most of the quenching events in our model. Up toblack hole masses of about $10^{8.5}\,{\rm M}_\odot$, the dominant growthchannel for SMBHs is in the thermal mode. Higher mass black holes stay mainlyin the kinetic mode and gas accretion is self-regulated via their feedback,which causes their Eddington ratios to drop, with SMBH mergers becoming themain channel for residual mass growth. As a consequence, the quasar luminosityfunction is dominated by rapidly accreting, moderately massive black holes inthe thermal mode. We show that the associated growth history of SMBHs producesa low-redshift quasar luminosity function and a redshift zero black holemass-stellar bulge mass relation in good agreement with observations, whereasthe simulation tends to over-predict the high-redshift quasar luminosityfunction.

Supermassive black holes and their feedback effects in the IllustrisTNG simulation