Observations of obscured quasars such as SDSS J1356+1026 have revealed outflows extending out to tens of kiloparsecs from the galactic nucleus [@Greene2012]. The estimated mechanical luminosity of these outflows ($10^{44-45}$ ergs s$^{-1}$) is too large to be explained by the inferred star formation activity. Other obscured quasars possess more massive outflows, with mass-loss rates of hundreds of solar masses per year [@Moe2009; @Dunn2010]. Meanwhile, observations of local ultra-luminous infrared galaxies (ULIRGs) have led to the discovery of outflows with velocities that are correlated with the AGN bolometric luminosity [@Sturm2011]. These outflows also have mass-loss rates equal to several times the star formation rate and in some cases exceeding 1000 solar masses per year, depleting the gas on timescales as short as $10^6$ years. Adding to our picture are studies of post-starburst galaxies, exhibiting outflows with median velocity of approximately 1000 km s$^{-1}$, suggesting that past AGN activity played a role in launching the gas [@Tremonti2007].

These observations are complemented by numerical simulations of AGN feedback [@Ciotti2010; @DeBuhr2011-1; @DeBuhr2011-2] that account for deposition of both energy and momentum from the accretion radiation, including a combination of heating by X-rays and photoionizations, radiation pressure at the kiloparsec scale, and winds driven from 