Spectroscopic Identifications for a Big Faint z=3.3--5.0 Quasar Sample

Details Spectroscopic Identifications for a Big Faint z=3.3--5.0 Quasar Sample Spectroscopic Identifications for a Big Faint z=3.3--5.0 Quasar Sample

Feb 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999noao.prop..387h&link_type=abstract

NOAO Proposal ID #1999A-0387

Computer Science

Scientific paper

Faint quasar surveys are a necessary complement to bright surveys to enable separation of redshift and luminosity dependencies in quasar properties. Such surveys can also put strong constraints on massive galaxy formation models and on the quasar contribution to the UV and x-ray backgrounds by determining %through the determination of the faint-end slope of the quasar luminosity function (QLF) and its evolution from z=3.3-5. We have completed a 7 deg^2 %** BRI imaging survey for faint z=3.3-5 quasars with the CTIO4m + BTC. Our deep imaging enables candidate selection %We can select candidates to R=23.5, equivalent to %M_B=- 23 at z=3.3-4 and M_B=-23.5 at z=4-5. We expect to find 115-220 z=3.3-4 and 13-40 z=4-5 quasars, enough to define the faint end of the z> 3.3 QLF as accurately as the bright end is currently known. We propose to begin spectroscopy of candidates with R< 23 %** using HYDRA- CTIO in parallel with HYDRA-WIYN. We have enough candidates per field that fibers are more efficient than longslit spectroscopy, and we will also target B-band dropout galaxies to R=22. This survey will provide a sample of faint high-z quasars suitable for detailed spectroscopic studies of quasar emission properties %-as f(z,L) with Gemini, as well as studies of intervening absorbers, quasar host galaxies, and large-scale structure at z> 3.3.

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