  We measure the 2-point correlation function, xi(AG), between galaxies and
quasar absorption line systems at z<1, using the dataset of Morris & Jannuzi
(2006; paper I) on 16 lines of sight (LOS) with UV spectroscopy and galaxy
multi-object spectroscopy. The measurements are made in 2-D redshift space out
to pi=20/h Mpc (comoving) along the LOS and out to 2/h Mpc projected; as a
function of HI column density in the range N(HI) = 1E13-1E19 cm^-2, for CIV
systems and as a function of galaxy spectral type. This extends the
absorber-galaxy pair count analysis of paper I. We find that the peak amplitude
of xi(AG) at the smallest separations increases slowly as the lower limit on
N(HI) is increased from 1E13 to 1E16 cm^-2, and then jumps sharply (albeit with
substantial uncertainty) at N(HI)>1E17 cm^-2. For CIV absorbers, the peak
strength of xi(AG) is comparable to that of HI absorbers with N(HI)>1E16.5
cm^-2.
  We do not reproduce the differences reported by Chen et al. between 1-D
xi(AG) measurements using galaxy sub-samples of different spectral types, but
the full impact of systematic differences in our samples is hard to quantify.
We compare the observations with smoothed particle hydrodynamical (SPH)
simulations and discover that in the observations xi(AG) is more concentrated
to the smallest separations than in the simulations. The latter also display a
`finger of god' elongation of xi(AG) along the LOS in redshift space, which is
absent from our data, but similar to that found by Ryan-Weber for the
cross-correlation of quasar absorbers and HI-emission-selected galaxies. The
physical origin of these `fingers of god' is unclear and we highlight several
possible areas for further investigation.
