density cylindrical shell, and @Krolik2007 extended that work to account for a more self-consistent rearrangement of the gas under the influence of the radiation. A radiation-hydrodynamics study that linked the effects of Compton scattering and broad absorption line winds at the parsec scale with inflow processes on galactic (kiloparsec) scales in two spatial dimensions was undertaken by @Novak2011, and this was extended in order to capture the radiative transfer through dusty gas in @Novak2012. Our study extends this work further by performing three dimensional Monte Carlo radiative transfer calculations for dusty gas, including both smooth and clumpy gas distributions, and by integrating the force on columns of gas in order to quantify the mass outflow rate from AGN radiating at high luminosity.

The momentum flux in radiation from a SMBH accretion disk with luminosity $L$ is $L/c$. Generally $L$ will not exceed $L_\mathrm{Edd}$, the Eddington luminosity set by the electron scattering (Thomson) opacity. Dust will contribute to the opacity seen by the radiation at large radii, but only at distances greater than the radius $r_\mathrm{sub}$ at which its temperature drops below the sublimation temperature $T_\mathrm{sub} \approx 1400 \; \mathrm{K}$. Although the sublimation temperature varies for each grain depending on its 