An Ultraviolet Extension to a Large Imaging Survey

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We propose to use the Mosaic and Mosaic2 cameras on the KPNO and CTIO 4m telescopes for U band photometry of 40 square degrees of sky, as a complement to the recently completed BTC survey (six fields in the B,V,I and z bands). Eight nights of 4m dark time in semester 1999B and six dark nights in semester 2000A are requested, to reach a 5σ limit of U=25.3. The ultraviolet imaging will be used to add new scientific capabilities to the BTC database. One goal is the multicolor selection of over 16,000 quasar candidates over the entire redshift range of 0 < z < 5. The U-B baseline is essential for the most efficient selection of quasars at z < 2. Selective spectroscopic follow-up will use upcoming 6-8m class telescopes, and HST for the brighter targets. The brighter quasars will be used to set up a grid of absorption line probes to compare with large scale structure as defined by galaxies and clusters. The faint quasars will be used for a clustering and luminosity function analysis. Another goal is the selection of low redshift star-forming galaxies and high redshift Lyman ``drop-out'' galaxies. The U band increases both the precision and the reliability of photometric redshifts. Reduced data and object catalogs will be made publicly available after 12 months, as with the BTC survey.

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