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A. Conti, A. Connolly (University of Pittsburgh)
With the new generation of deep, space-based imaging surveys, such as those proposed for the SNAP satellite, we will have an unprecedented opportunity to characterize the evolution of the clustering properties of galaxies across a wide range of look-back times. We consider here the application of photometric redshift techniques to the study of the large-scale clustering of galaxies as a function of redshift and galaxy type. Given the proposed sensitivities of the SNAP instrumentation and the characteristics of the multicolor imaging surveys (filter design and survey geometry) we estimate the expected uncertainties (statistical and systematic) within the photometric redshift estimators (both current and future implementations) and how these uncertainties might be propagated through to clustering statistics. We discuss both the advantages and limitations of angular (and pseudo-3D) clustering statistics for measuring the 3D distribution of galaxies and show how these measures might be used to constrain galaxy formation models.