HIGH-RESOLUTION SPECTRA OF INTRINSIC ABSORPTION-LINES IN THE QUASI-STELLAR OBJECT UM-675

We discuss high-resolution (similar to 9 km s(-1)) Keck Observatory sp ectra of the associated (z(a) approximate to z(e)) absorption lines in the z(e) = 2.15 QSO UM 675. In a previous paper we showed that the ti me-variable absorption lines require a minimum gas density of similar to 4000 cm(-3) and a maximum distance of similar to 1 kpc from the QSO . We also inferred metallicities of Z greater than or similar to Z. fr om an assortment of measured column densities. The new data yield abso rption-line profiles for Ly alpha, and C IV, more reliable column dens ities, and evidence for partial coverage of the background emission so urce(s). The z(a) approximate to z(e) line profiles are dominated by b road (FWHM approximate to 470 km s(-1)) and relatively smooth componen ts with centroids shifted roughly -1500 hm s(-1) from the emission-lin e redshift. Much weaker narrow-line components (with FWHM approximate to 55 and 29 km s(-1)) are also detected inside the broad C IV and N V profiles, but they contribute negligibly to the total equivalent widt hs and column densities. The complex of broad and narrow lines indicat es formation in an outflow, possibly in discrete ejection events, wher e distinct regions have the same outflow velocity but different (nonth ermal) velocity dispersions. The doublet ratios in C IV indicate that its broad and narrow components both cover less than 50% of the emissi on source(s). This is further strong evidence for absorption near the QSO by clouds that ape less than or similar to 0.1 pc across. In contr ast, the Ly alpha absorber covers greater than or similar to 83% of th e emission source(s) and O VI covers greater than or similar to 60%, i ndicating that different ions can have different coverage fractions. S caling air of the metallic column densities upward by amounts appropri ate for the C IV coverage fraction implies a metallicity of greater th an or similar to 2 Z.. However, the metallicity could be much lower if large H I columns are ''hidden'' in the Ly alpha profile.