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          Institute: MPI für Astrophysik     Collection: Cosmology     Display Documents

ID: 10977.0, MPI für Astrophysik / Cosmology
Galaxy clustering in early Sloan Digital Sky Survey redshift data
Authors:Zehavi, I.; Blanton, M. R.; Frieman, J. A.; Weinberg, D. H.; Mo, H. J.; Strauss, M. A.; Anderson, S. F.; Annis, J.; Bahcall, N. A.; Bernardi, M.; Briggs, J. W.; Brinkmann, J.; Burles, S.; Carey, L.; Castander, F. J.; Connolly, A. J.; Csabai, I.; Dalcanton, J. J.; Dodelson, S.; Doi, M.; Eisenstein, D.; Evans, M. L.; Finkbeiner, D. P.; Friedman, S.; Fukugita, M.; Gunn, J. E.; Hennessy, G. S.; Hindsley, R. B.; Ivezic, Z.; Kent, S.; Knapp, G. R.; Kron, R.; Kunszt, P.; Lamb, D. Q.; Leger, R. F.; Long, D. C.; Loveday, J.; Lupton, R. H.; McKay, T.; Meiksin, A.; Merrelli, A.; Munn, J. A.; Narayanan, V.; Newcomb, M.; Nichol, R. C.; Owen, R.; Peoples, J.; Pope, A.; Rockosi, C. M.; Schlegel, D.; Schneider, D. P.; Scoccimarro, R.; Sheth, R. K.; Siegmund, W.; Smee, S.; Snir, Y.; Stebbins, A.; Stoughton, C.; SubbaRao, M.; Szalay, A. S.; Szapudi, I.; Tegmark, M.; Tucker, D. L.; Uomoto, A.; Berk, D. V.; Vogeley, M. S.; Waddell, P.; Yanny, B.; York, D. G.
Date of Publication (YYYY-MM-DD):2002
Title of Journal:The Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Issue / Number:1
Start Page:172
End Page:190
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present the first measurements of clustering in the Sloan Digital Sky Survey (SDSS) galaxy redshift survey. Our sample consists of 29,300 galaxies with redshifts 5700 km s(-1) less than or equal to cz less than or equal to 39, 000 km s(-1), distributed in several long but narrow (2.degrees5-5degrees) segments, covering 690 deg(2). For the full, flux-limited sample, the redshift-space correlation length is approximately 8 h(-1) Mpc. The two-dimensional correlation function xi(r(p), pi) shows clear signatures of both the small-scale, "fingers- of-God" distortion caused by velocity dispersions in collapsed objects and the large-scale compression caused by coherent flows, though the latter cannot be measured with high precision in the present sample. The inferred real-space correlation function is well described by a power law, xi(r) = (r/6.1 +/- 0.2 h(-1) Mpc)(-1.75 +/- 0.03), for 0.1 h(-1) Mpc less than or equal to r less than or equal to 16 h(-1) Mpc. The galaxy pair- wise velocity dispersion is sigma(12) approximate to 600 +/- 100 km s(-1) for projected separations 0.15 h(-1) Mpc less than or equal to r(p) less than or equal to5 h(-1) Mpc. When we divide the sample by color, the red galaxies exhibit a stronger and steeper real-space correlation function and a higher pairwise velocity dispersion than do the blue galaxies. The relative behavior of subsamples defined by high/low profile concentration or high/low surface brightness is qualitatively similar to that of the red/blue subsamples. Our most striking result is a clear measurement of scale-independent luminosity bias at r less than or similar to 10 h(-1) Mpc: subsamples with absolute magnitude ranges centered on M-* - 1.5, M-*, and M-* + 1.5 have real-space correlation functions that are parallel power laws of slope approximate to -1.8 with correlation lengths of approximately 7.4, 6.3, and 4.7 h(-1) Mpc, respectively.
Free Keywords:cosmology : observations; cosmology : theory; dark matter; galaxies : clusters : general; galaxies : distances and redshifts; large-scale structure of universe
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astrophysik
External Affiliations:Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA; Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA; Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA; NYU, Dept Phys, New York, NY 10003 USA; Ohio State Univ, Dept Astron, Columbus, OH 43210 USA; Max Planck Inst Astrophys, D-85741 Garching, Germany; Princeton Univ Observ, Princeton, NJ 08544 USA; Univ Washington, Dept Astron, Seattle, WA 98195 USA; Univ Chicago, Yerkes Observ, Williams Bay, WI 53191 USA; Apache Point Observ, Sunspot, NM 88349 USA; Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA; Lorand Eotvos Univ, Dept Phys, H-1518 Budapest, Hungary; Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA; Univ Tokyo, Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan; Univ Tokyo, Inst Astron, Tokyo 1130033, Japan; Univ Arizona, Steward Observ, Tucson, AZ 85721 USA; Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan; USN Observ, Washington, DC 20392 USA; USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA; CERN, IT Div, CH-1211 Geneva 23, Switzerland; Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA; Univ Sussex, Sussex Astron Ctr, Brighton BN1 9QJ, E Sussex, England; Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA; Univ Edinburgh, Dept Phys & Astron, Edinburgh EH9 3JZ, Midlothian, Scotland; CALTECH, Dept Astron, Pasadena, CA 91125 USA; Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA; Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA; Univ Maryland, Dept Astron, College Pk, MD 20742 USA; Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA; Univ Penn, Dept Phys, Philadelphia, PA 19101 USA; Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA
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