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V.E. Margoniner (UC Davis), A. Connolly (U. Pittsburgh), J.A. Tyson (UC Davis)
Characterizing the redshift distribution of galaxies plays a fundamental role in the de-projection of the 2-dimensional distribution of galaxies on the sky into the real 3-dimensional Universe, as well as in any study of galaxy evolution, and in most known methods useful in constraining cosmological parameters. A great strength of LSST is that from its ugrizy deep photometry we will be able to derive redshifts for each galaxy with a typical precision of ~ 0.07(1+z) without any priors. Better precision may be obtained by adding combinations of magnitude and surface brightness priors or red sequence. We show from simulations and from existing HDFN data in similar photometric bands how this precision will be achieved, and we quantify the magnitude and impact of any redshift-dependent bias. The color-z errors are not Gaussian, and we discuss modeling methods and calibration using a combination of selected area deep spectroscopic samples and optical+IR many band photo-z.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.