The SDSS Quasar Survey: Quasar Luminosity Function from Data Release Three

Details The SDSS Quasar Survey: Quasar Luminosity Function from Data Release Three The SDSS Quasar Survey: Quasar Luminosity Function from Data Release Three

2006-01-19

arxiv.org/abs/astro-ph/0601434v2

Astron.J.131:2766-2787,2006

Astronomy and Astrophysics

Astrophysics

57 pages, 21 figures (9 color); minor changes to reflect the version accepted by AJ; higher resolution version available at

Scientific paper

10.1086/503559

We determine the number counts and z=0-5 luminosity function for a well-defined, homogeneous sample of quasars from the Sloan Digital Sky Survey (SDSS). We conservatively define the most uniform statistical sample possible, consisting of 15,343 quasars within an effective area of 1622 deg^2 that was derived from a parent sample of 46,420 spectroscopically confirmed broad-line quasars in the 5282 deg^2 of imaging data from SDSS Data Release Three. The sample extends from i=15 to i=19.1 at z<3 and to i=20.2 for z>3. The number counts and luminosity function agree well with the results of the 2dF QSO Survey, but the SDSS data probe to much higher redshifts than does the 2dF sample. The number density of luminous quasars peaks between redshifts 2 and 3, although uncertainties in the selection function in this range do not allow us to determine the peak redshift more precisely. Our best fit model has a flatter bright end slope at high redshift than at low redshift. For z<2.4 the data are best fit by a redshift-independent slope of beta = -3.1 (Phi(L) propto L^beta). Above z=2.4 the slope flattens with redshift to beta=-2.37 at z=5. This slope change, which is significant at a >5-sigma level, must be accounted for in models of the evolution of accretion onto supermassive black holes.

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