High-velocity outflows in quasars

High-velocity (HV) outflows are an important but poorly understood aspect of quasar/SMBH evolution. Outflows during the luminous accretion phase might play a critical role in "unveiling" young dusty AGN and regulating star formation in the host galaxies. Most quasar studies have focused on the broad absorption lines (BALs). We are involved in a program to study a nearly unexplored realm of quasar outflow parameter space: HV winds with upsilon > 10, 000 km/s (up to upsilon approximate to 0.2c) but small velocity dispersions (narrow absorption lines), such that Delta upsilon/upsilon << 1. Narrow-line HV flows merit specific attention because they complement the BAL work and pose unique challenges for models of the wind acceleration, mass loss rates, launch radii, geometry, etc. We have selected the brightest quasars at 1.8 < z < 3.5 with candidate narrow HV outflow lines (CIV 1548 angstrom) in existing SDSS spectra and followed up with monitoring observations to i) characterize, for the first time, the variability in a sample of absorbers spanning a wide range of velocities and FWHMs, including some marginal BALs, ii) identify/confirm more of the true outflow systems, e.g., among the more ambiguous narrow lines, and iii) test the wind models and derive better constraints on basic outflow properties, such as the kinematics, locations, and physical conditions.