Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 424, Issue 2, Pages 933-950Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2012.21251.x
Keywords
quasars: general; cosmology: observations; large-scale structure of Universe
Categories
Funding
- Alfred P. Sloan Foundation
- Participating Institutions
- National Science Foundation
- US Department of Energy Office of Science
- NSF
- NASA [HST-HF-51285.01]
- Spanish grants [AYA2009-09745, PR2011-0431]
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- University of Cambridge
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- ICREA Funding Source: Custom
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [806861] Funding Source: National Science Foundation
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We measure the quasar two-point correlation function over the redshift range 2.2 < z < 2.8 using data from the Baryon Oscillation Spectroscopic Survey. We use a homogeneous subset of the data consisting of 27 129 quasars with spectroscopic redshifts by far the largest such sample used for clustering measurements at these redshifts to date. The sample covers 3600 deg(2), corresponding to a comoving volume of 9.7 (h(-1) Gpc)(3) assuming a fiducial Lambda cold dark matter cosmology, and it has a median absolute i-band magnitude of -26, k-corrected to z= 2. After accounting for redshift errors we find that the redshift-space correlation function is fitted well by a power law of slope -2 and amplitude s(0)=(9.7 +/- 0.5)h(-1) Mpc over the range 3 < s < 25 h(-1) Mpc. The projected correlation function, which integrates out the effects of peculiar velocities and redshift errors, is fitted well by a power law of slope -1 and r(0)=(8.4 +/- 0.6)h(-1) Mpc over the range 4 < R < 16 h(-1) Mpc. There is no evidence for strong luminosity or redshift dependence to the clustering amplitude, in part because of the limited dynamic range in our sample. Our results are consistent with, but more precise than, previous measurements at similar redshifts. Our measurement of the quasar clustering amplitude implies a bias factor of b similar or equal to 3.5 for our quasar sample. We compare the data to models to constrain the manner in which quasars occupy dark matter haloes at z similar to 2.4 and infer that such quasars inhabit haloes with a characteristic mass of < M > similar or equal to 10(12) h(-1) M-circle dot with a duty cycle for the quasar activity of 1 per cent.
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