Radiation pressure-driven outflows from dusty AGN

TL;DR

This study uses radiation simulations to explore how dust properties and AGN characteristics influence radiation pressure-driven outflows from supermassive black holes, revealing key factors affecting AGN feedback and outflow boundaries.

Contribution

It provides a detailed analysis of how dust abundance, AGN properties, and other factors affect radiation-driven outflows using CLOUDY simulations, highlighting the dominant role of dust in feedback processes.

Findings

Dust abundance significantly impacts feedback efficiency.

Inner radius and shell width have minor effects.

Presence of nuclear star clusters reduces feedback effectiveness.

Abstract

Radiation pressure-driven outflows from luminous accreting supermassive black holes are an important part of active galactic nucleus (AGN) feedback. The effective Eddington limit, based on absorption of radiation by dust, not electron scattering, is revealed in the plane of AGN absorption column density $N_{\mathrm{H}}$ as a function of Eddington fraction $\lambda_{\mathrm{Edd}} = L_{\mathrm{bol}}/L_{\mathrm{Edd}}$, where a lack of objects is seen in the region where the effective limit is exceeded. Here, we conduct radiation simulation using the CLOUDY code to deduce the radiative force applied onto dusty gas at the nucleus and compare to the gravitational force to reveal the outflow region and its boundary with long-lived absorption clouds. We also investigate how the outflow condition is affected by various AGN and dust properties and distribution. As expected, the dust abundance has the largest effect on the $N_{\mathrm{H}} - \lambda_{\mathrm{Edd}}$ diagram since the higher the abundance, the more effective the radiative feedback, while the impact of the inner radius of the dusty gas shell, the shell width and the AGN spectral shape are relatively negligible. The presence of other central masses, such as a nuclear star cluster, can also make the feedback less effective. The AGN spectral energy distribution depends on the mass of the black hole and its spin. Though the effects of the AGN SED on the diagram are relatively small, the fraction of ionizing ultraviolet (UV) photons from the blackbody accretion disc is affected more by black hole mass than spin, and can influence the efficiency of radiation pressure.