A sample of faint, V magnitude selected, galaxy pairs, having physical separations less than approximately 20h −1 kpc, 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 ≤ 22.5) that are in close (θ < 6 ′′ ) 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 ≤ 22.5 field population is 0.36, statistically equal to the average redshift of 0.42 for the pairs. The similarity of the two redshift distributions, ∆z ≤ 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 θ ≤6 ′′ higher than the inward extrapolation of ω(θ) ∝ θ −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 ± 0.8. If all pairs at low velocities and r ≤ 20h −1 kpc merge, then the average galaxy mass would be 32% smaller at z = 0.4 than locally.