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We study the effects of a detailed dust treatment on the properties andevolution of early-type galaxies containing central black holes, as determinedby AGN feedback. We find that during cooling flow episodes, radiation pressureon the dust in and interior to infalling shells of cold gas can greatly impactthe amount of gas able to be accreted and therefore the frequency of AGNbursts. However, the overall hydrodynamic evolution of all models, includingmass budget, is relatively robust to the assumptions on dust. We find that IRre-emission from hot dust can dominate the bolometric luminosity of the galaxyduring the early stages of an AGN burst, reaching values in excess of $10^{46}$erg/s. The AGN-emitted UV is largely absorbed, but the optical depth in the IRdoes not exceed unity, so the radiation momentum input never exceeds $L_{\rmBH}/c$. We constrain the viability of our models by comparing the AGN dutycycle, broadband luminosities, dust mass, black hole mass, and other modelpredictions to current observations. These constraints force us to modelswherein the dust to metals ratios are $\simeq 1%$ of the Galactic value, andonly models with a dynamic dust to gas ratio are able to produce both quiescentgalaxies consistent with observations and high obscured fractions during AGN"on" phases. During AGN outbursts, we predict that a large fraction of the FIRluminosity can be attributed to warm dust emission ($\simeq100$ K) from densedusty gas within $\leq 1$ kpc reradiating the AGN UV emission.

Grain Physics and IR Dust Emission in AGN Environments