The Infrared Emission and Opening Angle of the Torus in Quasars

TL;DR

This study analyzes the infrared emission and geometry of the dusty torus in quasars, revealing its significant contribution to infrared luminosity and its dependence on accretion rate, supporting the unified model of AGNs.

Contribution

It provides detailed spectral decomposition of quasar infrared emission, linking torus properties to accretion rates and refining the understanding of torus geometry in AGNs.

Findings

Torus contributes ~70% of infrared luminosity.

Torus opening angle decreases with accretion rate up to Eddington ratio 0.5.

Most quasars have mildly inclined tori, consistent with the unified model.

Abstract

According to the unified model of active galactic nuclei (AGNs), a putative dusty torus plays an important role in determining their external appearance. However, very limited information is known about the physical properties of the torus. We perform detailed decomposition of the infrared ($1-500\,\mu$m) spectral energy distribution of 76 $z < 0.5$ Palomar-Green quasars, combining photometric data from 2MASS, WISE, and Herschel with Spitzer spectroscopy. Our fits favor recent torus spectral models that properly treat the different sublimation temperatures of silicates and graphite and consider a polar wind component. The AGN-heated dust emission from the torus contributes a significant fraction ($\sim 70\%$) of the total infrared ($1-1000\, \mu$m) luminosity. The torus luminosity correlates well with the strength of the ultraviolet/optical continuum and the broad $\rm{H\beta}$ emission line, indicating a close link between the central ionization source and re-radiation by the torus. Consistent with the unified model, most quasars have tori that are only mildly inclined along the line-of-sight. The half-opening angle of the torus, a measure of its covering factor, declines with increasing accretion rate until the Eddington ratio reaches $\sim 0.5$, above which the trend reverses. This behavior likely results from the change of the geometry of the accretion flow, from a standard geometrically thin disk at moderate accretion rates to a slim disk at high accretion rates.