  A sample of faint, V magnitude selected, galaxy pairs, having physical
separations less than approximately 20\hkpc, is used to examine the rise in the
merger rate with redshift and the statistical relations between close pairs and
the field galaxy population. Redshifts have been obtained for 14 galaxies ($V
\le 22.5$) that are in close ($\theta < 6\arcs$) pairs, along with a comparison
sample of 38 field galaxies. Two color photometry is available for about 1000
galaxies in the same fields. The average redshift of the $V\le22.5$ field
population is 0.36, statistically equal to the average redshift of 0.42 for the
pairs. The similarity of the two redshift distributions, $\Delta z\le 0.1$,
limits any differential luminosity enhancement of close pairs to less than half
a magnitude. The pairs are somewhat bluer than the field and have nearly twice
the average [O~II] detection rate of the field, but the differences are not
statistically significant. The field population has an angular correlation at
separations of $\theta\le$6\arcs\ higher than the inward extrapolation of
$\omega(\theta)\propto \theta^{-0.8}$, which may be a population of
``companions'' not present at the current epoch, or, luminosity enhancement of
intrinsically faint galaxies in pairs. Physical pairs comprise about 7\% of the
faint galaxies in our survey fields. The same physical separation applied to
local galaxies finds only 2.6\% in pairs. If the rise in close low relatively
velocity pairs with redshift is parameterized as $(1+z)^m$, then $m=2.9\pm0.8$.
If all pairs at low velocities and $r\le 20$\hkpc\ merge, then the
