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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 ◦ 5 × 0 ◦ 5 fields were observed for a total of 2 hours each in I and V, resulting in catalogs containing ∼ 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 Awθ −δ, and find ω(θ) to be well described by a power-law of index δ = 0.8. We find the amplitude of the correlation function, Aw, 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 ǫ parameter inadequately describe the observations. This is because the predictions do not allow for the varying mix of morphologies and absolute luminosities (and hence clusterin

Year: 2002

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