Population synthesis of active galactic nuclei based on the radiation-regulated unification model

TL;DR

This study uses simulation-based inference with ray-tracing to model the X-ray emission of AGNs, aiming to reproduce observed X-ray backgrounds and properties, and constrains the physical structure of the AGN population.

Contribution

It introduces a self-consistent, simulation-based approach to model AGN properties and their X-ray emission, incorporating the radiation-regulated unification model.

Findings

Derived an intrinsic Compton-thick fraction of 40±3%.

Reproduced the cosmic X-ray background and AGN counts with the model.

Constrained the size and density of the dusty torus in AGNs.

Abstract

X-ray surveys of active galactic nuclei (AGNs) provide direct constraints on the properties of individual AGNs, such as their emission, obscuration, and accretion rate. Previous AGN population synthesis models have not addressed such properties self-consistently. Here, we use a simulation-based inference (SBI) approach to constrain the geometrical and physical properties of the AGN population. We perform numerical simulations with our ray-tracing code, RefleX, which allows the self-consistent modelling of the X-ray emission of AGNs with flexible circumnuclear and source geometries. We create our synthetic population by sampling the intrinsic active black hole mass function (BHMF) and Eddington ratio distribution function (ERDF) of local AGNs, and we construct a geometry based on the radiation-regulated model, along with Eddington-ratio-dependent emission spectra. Using the RefleX-simulated emission of the AGN population, we aim to simultaneously reproduce the cosmic X-ray background (CXB), differential AGN number counts, and several observed absorption properties of local AGNs, such as the fraction of $N_\mathrm{H}$ in bins of log($N_\mathrm{H}$), the Compton-thick fraction as a function of limiting flux, and the number of obscured and unobscured AGNs as a function of Eddington ratio. With this approach, we test the consistency of the radiation-regulated model with a very comprehensive set of X-ray observables, while constraining the size and density of the dusty torus and the evolution of the local AGN population. We derive an intrinsic Compton-thick fraction of $40\pm3$%, and find that a simple evolutionary prescription controlling the active fraction of supermassive black holes is sufficient for our synthetic population to reproduce the CXB.