  We present a preliminary measurement of the angular clustering of faint ($R
\le 25$) field galaxies in which we concentrate on the behavior of $w(\theta)$
on small angular scales ($\theta \ls 10''$). The galaxies are strongly
clustered and $w(\theta)$ is well-characterized by a power law of the form $A_w
\theta^{-\delta}$. The best-fitting value of the power law index, $\delta$, is,
however, steeper than the fiducial value of $\delta = 0.8$, indicating there
are more pairs of galaxies separated by $\theta \ls 10''$ in our sample than
would be otherwise expected. Using the best-fitting form of $w(\theta)$, we
estimate that $\sim 10%$ of the galaxies are in physically close pairs
(separations $\ls 21 h^{-1}$ kpc). This is a factor of order 2 larger than
local galaxy samples, but comparable to galaxy samples with $<z> \sim 0.4$. The
mean redshift of our galaxies is of order 0.95, and, therefore, our result
suggests that there was little or no evolution in the merger rate of galaxies
between $z \sim 1$ and $z \sim 0.4$.
