Measuring the evolution in the clustering of galaxies over a large redshift range is a challenging problem .
We have developed a new technique which uses photometric redshifts to measure the angular correlation function in redshift shells .
This novel approach minimizes the galaxy projection effect inherent in standard angular correlation measurements , and allows for a measurement of the evolution in the galaxy correlation strength with redshift .
In this paper , we present new results which utilize more accurate photometric redshifts , which are derived from a multi-band dataset ( U , B , R , and I ) covering almost two hundred square arcminutes to B _ { AB } \sim 26.5 ^ { m } , to quantify the evolution in the clustering of galaxies for z < 1 .
We also extend our technique to incorporate absolute magnitudes , which provides a simultaneous measurement of the evolution of clustering with both redshift and intrinsic luminosity .
Specifically , we find a gradual decline in the strength of clustering with redshift out to z \sim 1 , as predicted by semi-analytic models of structure formation .
Furthermore , we find that r _ { 0 } ( z = 0 ) \approx 4.0 h ^ { -1 } Mpc for the predictions of linear theory in an \Omega _ { 0 } = 0.1 universe .