The effect of radiation pressure on dusty absorbing gas around AGN

TL;DR

This paper investigates how radiation pressure on dusty gas influences AGN obscuration and feedback, showing that dust significantly amplifies radiation pressure effects, which can explain observed AGN properties and black hole-galaxy relations.

Contribution

It introduces a model quantifying radiation pressure enhancement on dusty gas and demonstrates its consistency with observed AGN distributions and galaxy-black hole relations.

Findings

Radiation pressure on dusty gas can be 1 to 500 times stronger than Thomson scattering.

AGN with certain column densities match the predicted distribution based on radiation pressure effects.

The model explains the black hole mass - bulge mass relation and AGN feedback mechanisms.

Abstract

Many Active Galactic Nuclei (AGN) are surrounded by gas which absorbs the radiation produced by accretion onto the central black hole and obscures the nucleus from direct view. The dust component of the gas greatly enhances the effect of radiation pressure above that for Thomson scattering so that an AGN which is sub-Eddington for ionized gas in the usual sense can appear super-Eddington for cold dusty gas. The radiation-pressure enhancement factor depends on the AGN spectrum but ranges between unity and about 500, depending on the column density. It means that an AGN for which the absorption is long-lived should have a column density N_H>5x10^23 lambda cm^-2, where lambda is its Eddington fraction L_bol/L_Edd, provided that N_H}>5x10^21 cm^-2. We have compared the distribution of several samples of AGN - local, CDFS and Lockman Hole - with this expectation and find good agreement. We show that the limiting enhancement factor can explain the black hole mass - bulge mass relation and note that the effect of radiation pressure on dusty gas may be a key component in the feedback of momentum and energy from a central black hole to a galaxy.