Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 308597.0, MPI für Astronomie / Publikationen_mpia
The Sloan Digital Sky Survey quasar survey: Quasar luminosity function from data release 3
Authors:Richards, G. T.; Strauss, M. A.; Fan, X.; Hall, P. B.; Jester, S.; Schneider, D. P.; Vanden Berk, D. E.; Stoughton, C.; Anderson, S. F.; Brunner, R. J.; Gray, J.; Gunn, J. E.; Ivezic, Z.; Kirkland, M. K.; Knapp, G. R.; Loveday, J.; Meiksin, A.; Pope, A.; Szalay, A. S.; Thakar, A. R.; Yanny, B.; York, D. G.; Barentine, J. C.; Brewington, H. J.; Brinkmann, J.; Fukugita, M.; Harvanek, M.; Kent, S. M.; Kleinman, S. J.; Krzesinski, J.; Long, D. C.; Lupton, R. H.; Nash, T.; Neilsen, E. H.; Nitta, A.; Schlegel, D. J.; Snedden, S. A.
Date of Publication (YYYY-MM-DD):2006
Journal Abbrev.:The Astronomical Journal
Volume:131
Start Page:2766
End Page:2787
Audience:Not Specified
Abstract / Description: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 deg2 that was derived from a parent sample of 46,420 spectroscopically confirmed broad-line quasars in the 5282 deg2 of imaging data from SDSS Data Release 3. The sample extends from i=15 to 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 Two Degree Field QSO Redshift Survey (2QZ) at redshifts and luminosities at which the SDSS and 2QZ quasar samples overlap, but the SDSS data probe to much higher redshifts than does the 2QZ 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)~Lbeta]. Above z=2.4 the slope flattens with redshift to beta>~-2.37 at z=5. This slope change, which is significant at the >~5 sigma level, must be accounted for in models of the evolution of accretion onto supermassive black holes.
Free Keywords:Cosmology: Observations; Galaxies: Active; Galaxies: Luminosity Function; Mass Function; Galaxies: Quasars: General; Surveys
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bi...
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.