Abstract. While the strategy for the first applications of weak lensing has been to “go deep ” it is equally interesting to use one’s telescope time to instead “go wide”. The Sloan Survey (SDSS) provides a natural framework for a very wide area weak lensing survey. Probing of the mass distribution using the distortion of galaxy image shapes by the intervening gravitational field this mass produces is a powerful new technique for probing cosmological structure (Valdes et al., 1983; Tyson et al., 1990; Miralda-Escudé, 1991; Blandford et al., 1991; Kaiser, 1992). The “weak lensing ” technique will no doubt become one of the standard probes, on par with galaxy redshift surveys and maps of CMBR anisotropies. Except for small areas on the sky near distant rich clusters or very near galaxies, the image distortion is expected to be small and weak lensing is the appropriate technique. One must average over many galaxies to obtain a significant detection of the small image distortion; typically by measuring correlations in galaxy position-angles and thus the shear. Dee
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