THE PHYSICAL CONDITIONS OF THE INTRINSIC Nv NARROW ABSORPTION LINE SYSTEMS OF THREE QUASARS

We employ detailed photoionization models to infer the physical conditions of intrinsic narrow absorption line systems found in high-resolution spectra of three quasars at z = 2.6-3.0. We focus on a family of intrinsic absorbers characterized by Nv lines that are strong relative to the Ly alpha lines. The inferred physical conditions are similar for the three intrinsic Nv absorbers, with metallicities greater than 10 times the solar value (assuming a solar abundance pattern), and with high ionization parameters (log U similar to 0). Thus, we conclude that the unusual strength of the Nv lines results from a combination of partial coverage, a high ionization state, and high metallicity. We consider whether dilution of the absorption lines by flux from the broad emission line region can lead us to overestimate the metallicities and we find that this is an unlikely possibility. The high abundances that we infer are not surprising in the context of scenarios in which metal enrichment takes place very early on in massive galaxies. We estimate that the mass outflow rate in the absorbing gas (which is likely to have a filamentary structure) is less than a few M(circle dot) yr(-1) under the most optimistic assumptions, although it may be embedded in a much hotter, more massive outflow.