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Photoionization modeling of certain low-ionization broad absorption lines inquasars implies very compact (Delta R~0.01 pc), galaxy-scale (R kpc) absorbersblueshifted by several 1000 km s^-1. While these are likely signatures ofquasar outflows, the lifetimes of such compact absorbers are too short for themto be direct ejecta from a nuclear wind. Instead, I argue that the absorbingclouds must be transient and created in situ. Following arguments detailed byFaucher-Giguere, Quataert, & Murray (2011), I show that a model in which thecool absorbers form in radiative shocks arising when a quasar blast waveimpacts an interstellar cloud along the line of sight successfully explains thekey observed properties. Using this radiative shock model, the outflow kineticluminosities for three luminous quasars are estimated to be Edot,k~2-5% L_AGN(with corresponding momentum fluxes Pdot~2-15 L_AGN/c), consistent withfeedback models of the M-sigma relation. These energetics are similar to thoserecently inferred of molecular outflows in local ultra-luminous infraredgalaxies and in post-starburt winds, suggesting that active galactic nuclei(AGN) are capable of driving such outflows. Radiative shocks probably affectthe multiphase structure of outflows in a range of other systems, includingnarrower and higher-ionization quasar absorption lines, and compactintergalactic absorbers ejected by star formation and AGN activity.

Quasar Absorption Lines from Radiative Shocks: Implications for Multiphase Outflows and Feedback