AAS 205th Meeting, 9-13 January 2005
Session 167 Quasars and Blazars
Oral, Thursday, January 13, 2005, 2:00-3:30pm, Royal Palm 1-3

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[167.03] The SDSS-DR3 and 2dF-SDSS Quasar Luminosity Functions

G.T. Richards, M.A. Strauss (Princeton), S.M. Croom, M. Colless, J. Bland-Hawthorn, R.G. Sharp (AAO), B.J. Boyle (ATNF), X. Fan (Arizona), D.G. York (Chicago), P.J. Outram, T. Shanks, N. Ross (Durham), A. Meiksin (Edinburgh), S. Jester, C. Stoughton (Fermilab), A. Szalay (JHU), L. Miller (Oxford), D.P. Schneider, D.E. Vanden Berk (Penn State), R.C. Nichol (Portsmouth), A.D. Myers (Illinois), S.F. Anderson, Z. Ivezic (Washington), M. Drinkwater, K.A. Pimbblet, I.G. Roseboom (Queensland), SDSS Collaboration, 2SLAQ Collaboration

We present two complementary determinations of the quasar luminosity function (QLF) based on over 50,000 bright quasars from the SDSS-DR3 quasar catalog and over 5000 faint quasars from the 2dF-SDSS LRG and QSO survey (2SLAQ). With a limiting magnitude of i=19.1 (i=20.2 for z>3) the SDSS-DR3 sample does not reach the "break" in the z<2.2 QLF, but the data allow, for the first time, the determination of the QLF from z=0 to z=5 in a single survey. For z<2.2 the SDSS-DR3 number counts and QLF are in good agreement with the bright end of the QLF from the 2dF QSO Redshift Survey (2QZ). The 2SLAQ sample, on the other hand, is limited to UVX sources (z<3), but with a limit of g=21.85 extends over 2 magnitudes fainter than the "break" and 1 magnitude fainter than the 2QZ sample. We find good agreement with previous results from 2QZ except at the faint end, where the 2SLAQ data indicate a higher density of quasars and thus a steeper QLF slope.

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