  For faint photometric surveys our ability to quantify the clustering of
galaxies has depended on interpreting the angular correlation function as a
function of the limiting magnitude of the data. Due to the broad redshift
distribution of galaxies at faint magnitude limits the correlation signal has
been extremely difficult to detect and interpret. We introduce a new technique
for measuring the evolution of clustering. We utilize photometric redshifts,
derived from multicolor surveys, to isolate redshift intervals and calculate
the evolution of the amplitude of the angular 2-pt correlation function.
Applying these techniques to the the Hubble Deep Field we find that the shape
of the correlation function, at z=1, is consistent with a power law with a
slope of -0.8. For z>0.4 the best fit to the data is given by a model of
clustering evolution with a comoving r0 = 2.37 Mpc and eps = -0.4 +/- 0.5,
consistent with published measures of the clustering evolution. To match the
canonical value of r0 = 5.4 Mpc, found for the clustering of local galaxies,
requires a value of eps = 2.10 +/- 0.5 (significantly more than linear
evolution). The log likelihood of this latter fit is 4.15 less than that for
the r0 = 2.37 Mpc model. We, therefore, conclude that the parameterization of
the clustering evolution of (1+z)^-(3+eps) is not a particularly good fit to
the data.
