Speaker
Description
The study of the spectral energy distribution (SED) of active galactic nuclei (AGN) plays a very important role in several aspects of AGN, such as the physics of black hole (BH) accretion, AGN feedback, and AGN luminosity function (LF). In this work, we explain the observed AGN LF with the SED more physically considered. Specifically, we strictly study the accretion model for a wide range of the dimensionless accretion rate $\dot{m}(\equiv \dot{M}/\dot{M}_\mathrm{Edd})$, then calculate the structure of the accretion flow and the corresponding SED by specifying black hole mass $m(\equiv M_\mathrm{BH}/M_\odot)$ and accretion rate $\dot{m}$. Further, combing with the semi-analytical model of galaxy formation L-Galaxies and Millennium style dark matter simulation for the distribution of ($m, \dot{m}$) at different redshift, we calculate the bolometric, soft X-ray, hard X-ray, and optical/UV LF theoretically. Finally, by comparing with observations, we found a satisfactory agreement between our predictions and observational determined LFs for redshift $z<1$. For $z>1$, our model's prediction deviates from observed LFs. We argue that such deviation may arises from the inherent AGN feedback prescription of the cosmological simulation, and can be alleviated to some extent by exploring the effects of the microphysics (such as viscosity and chaotic magnetic field) of the accretion flow on the SED and therefore on the LF.
