A Physical Model for the Quasar Luminosity Function Evolution between Cosmic Dawn and High Noon

Modeling the evolution of the number density distribution of quasars through the quasar luminosity function (QLF) is critical to improving our understanding of the connection between black holes, galaxies, and their halos. Here we present a novel semiempirical model for the evolution of the QLF that is fully defined after the specification of a free parameter, the internal duty cycle, epsilon (DC), along with minimal other assumptions. All remaining model parameters are fixed upon calibration against the QLF at two redshifts, z = 4 and z = 5. Our modeling shows that the evolution at the bright end results from the stochasticity in the median quasar luminosity versus halo mass relation, while the faint end shape is determined by the evolution of the halo mass function (HMF) with redshift. Additionally, our model suggests the overall quasar density is determined by the evolution of the HMF, irrespective of the value of epsilon (DC). The z >= 4 QLFs from our model are in excellent agreement with current observations for all epsilon (DC), with model predictions suggesting that observations at z greater than or similar to 7.5 are needed to discriminate between different epsilon (DC). We further extend the model at z <= 4, successfully describing the QLF between 1 <= z <= 4, albeit with additional assumptions on sigma and epsilon (DC). We use the existing measurements of quasar duty cycle from clustering to constrain epsilon (DC), finding epsilon (DC) similar to 0.01 or epsilon (DC) greater than or similar to 0.1 dependent on observational data sets used for reference. Finally, we present forecasts for future wide-area surveys with promising expectations for the Nancy Grace Roman Telescope to discover N greater than or similar to 10, bright, m (UV) < 26.5 quasars at z similar to 8.