  We investigate the relationship between galaxies and metal-line absorption
systems in a large-scale cosmological simulation with galaxy formation. Our
detailed treatment of metal enrichment and non-equilibrium calculation of
oxygen species allow us, for the first time, to carry out quantitative
calculations of the cross-correlations between galaxies and O VI absorbers. We
find the following: (1) The cross-correlation strength depends weakly on the
absorption strength but strongly on the luminosity of the galaxy. (2) The
correlation distance increases monotonically with luminosity from ~0.5-1h^-1
Mpc for 0.1L* galaxies to ~3-5h^-1 Mpc for L* galaxies. (3) The correlation
distance has a complicated dependence on absorber strength, with a
luminosity-dependent peak. (4) Only 15% of O VI absorbers lie near >=Lz*
galaxies. The remaining 85%, then, must arise ``near'' lower-luminosity
galaxies, though, the positions of those galaxies is not well-correlated with
the absorbers. This may point to pollution of intergalactic gas predominantly
by smaller galaxies. (5) There is a subtle trend that for >~0.5Lz* galaxies,
there is a positive correlation between absorber strength and galaxy luminosity
in the sense that stronger absorbers have a slightly higher probability of
finding such a large galaxy at a given projection distance. For less luminous
galaxies, there seems to be a negative correlation between luminosity and
absorber strength.
