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Broad absorption lines (BALs) in quasar spectra identify high velocityoutflows that might exist in all quasars and could play a major role infeedback to galaxy evolution. The viability of BAL outflows as a feedbackmechanism depends on their kinetic energies, as derived from the outflowvelocities, column densities, and distances from the central quasar. Weestimate these quantities for the quasar, Q1413+1143 (redshift $z_e = 2.56$),aided by the first detection of PV $\lambda\lambda$1118,1128 BAL variability ina quasar. In particular, PV absorption at velocities where the CIV trough doesnot reach zero intensity implies that the CIV BAL is saturated and the absorberonly partially covers the background continuum source (with characteristic size<0.01 pc). With the assumption of solar abundances, we estimate that the totalcolumn density in the BAL outflow is log N_H > 22.3 (cm^-2). Variability in thePV and saturated CIV BALs strongly disfavors changes in the ionization as thecause of the BAL variability, but supports models with high-column density BALclouds moving across our lines of sight. The observed variability time of 1.6yr in the quasar rest frame indicates crossing speeds >750 km/s and a radialdistance from the central black hole of <3.5 pc, if the crossing speeds areKeplerian. The total outflow mass is ~4100 M_solar, the kinetic energy ~4x10^54erg, and the ratio of the outflow kinetic energy luminosity to the quasarbolometric luminosity is ~0.02 (at the minimum column density and maximumdistance), which might be sufficient for important feedback to the quasar'shost galaxy.

A Variable PV Broad Absorption Line and Quasar Outflow Energetics