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Understanding how Active Galactic Nuclei (AGN) evolve through cosmic timeallows us to probe the physical processes that control their evolution. We usean updated model for the evolution of masses and spins of supermassive blackholes (SMBHs), coupled to the latest version of the semi-analytical model ofgalaxy formation GALFORM using the Planck cosmology and a high resolutionMillennium style dark matter simulation to make predictions for AGN and SMBHproperties for $0 < z < 6$. We compare the model to the observed black holemass function and the SMBH versus galaxy bulge mass relation at $z=0$, andcompare the predicted bolometric, hard X-ray, soft X-ray and optical AGNluminosity functions to observations at $z < 6$, and find that the model is ingood agreement with the observations. The model predicts that at $z<2$ and$L_{\mathrm{bol}} < 10^{43} \mathrm{ergs^{-1}}$, the AGN luminosity function isdominated by objects accreting in an Advection Dominated Accretion Flow (ADAF)disc state, while at higher redshifts and higher luminosities the dominantcontribution is from objects accreting via a thin disc or at super-Eddingtonrates. The model also predicts that the AGN luminosity function at $z<3$ and$L_{\mathrm{bol}} < 10^{44} \mathrm{ergs^{-1}}$ is dominated by thecontribution from AGN fuelled by quiescent hot halo accretion, while at higherluminosities and higher redshifts, the AGN luminosity function is dominated bythe contribution from AGN fuelled by starbursts triggered by discinstabilities. We employ this model to predict the evolution of SMBH masses,Eddington ratios, and spins, finding that the median SMBH spin evolves verylittle for $0<z<6$.

The evolution of SMBH spin and AGN luminosities for $z<6$ within a semi-analytic model of galaxy formation