We present measurements of the two-point galaxy angular correlation function as a function of apparent magnitude , color , and morphology .
Our analysis utilizes images taken using the UH8K CCD mosaic camera on the CFHT .
Six 0 \arcdeg 5 \times 0 \arcdeg 5 fields were observed for a total of 2 hours each in I and V , resulting in catalogs containing \sim 25000 galaxies per field .
We present new galaxy number counts to limiting magnitudes of I = 24.0 and V = 25.0 .
We divide each passband sample into intervals of width one magnitude .
Within each magnitude interval , we parameterize the angular correlation function by A _ { w } \theta ^ { - \delta } , and find \omega ( \theta ) to be well described by a power-law of index \delta = 0.8 .
We find the amplitude of the correlation function , A _ { w } , to decrease monotonically with increasingly faint apparent magnitude .
We compare with predictions which utilize redshift distributions based on deep spectroscopic observations .
We conclude that simple redshift-dependent models which characterize evolution by means of the \epsilon parameter inadequately describe the observations .
This is because the predictions do not allow for the varying mix of morphologies and absolute luminosities ( and hence clustering strengths ) of galaxies sampled at different apparent magnitudes .
We find a strong clustering dependence on V - I color .
This is because galaxies of extreme color lie at similar redshifts and the angular correlation functions for these samples are minimally diluted by chance projections .
We find extremely red ( V - I = 3.0 ) galaxies ( likely early-type galaxies at z \sim 1 ) to have an A _ { \omega } about 10 times , and extremely blue ( V - I = 0.5 ) galaxies ( likely local late types ) to have an A _ { \omega } about 15 - 20 times higher than that measured for the full field population .

We then present the first attempt to investigate the redshift evolution of clustering , utilizing a population of galaxies of the same morphological type and absolute luminosity .
We study the dependence of \omega ( \theta ) on redshift for L _ { \star } early-type galaxies in the redshift range 0.2 < z < 0.9 .
Although uncertainties are large , we find the evolution in the clustering of these galaxies to be consistent with stable clustering [ \epsilon = 0 for a redshift dependence of the spatial correlation function , \xi ( r ) , parametererized as \xi ( r,z ) = { \left ( { r } / { r _ { 0 } } \right ) } ^ { - \gamma } ( 1 + z ) ^ { - ( 3 + \epsilon ) } ] .
We find L _ { \star } early-type galaxies to cluster slightly more strongly ( physical correlation length r _ { 0 } = 5.25 \pm 0.28 ~ { } { h } ^ { -1 } { Mpc } assuming \epsilon = 0 ) than the local full field population .
This is in good agreement with the correlation length measured by the 2dFGRS for L _ { \star } early-type galaxies in the local universe .