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Detection of the Baryon Acoustic Peak in the Large‐Scale Correlation Function of SDSS Luminous Red Galaxies

Daniel J. EisensteinAlfred P. Sloan FellowIdit ZehaviSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85121David W. HoggCenter for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003Roman ScoccimarroCenter for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003Michael R. BlantonCenter for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003Robert C. NicholInstitute of Cosmology and Gravitation, Mercantile House, Hampshire Terrace, University of Portsmouth, Portsmouth P01 2EG, UKRyan ScrantonDepartment of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260Hee‐Jong SeoSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85121Max TegmarkDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139Zheng ZhengSchool of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540Scott F. AndersonDepartment of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580Jim AnnisFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Neta BahcallPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Jon BrinkmannScott BurlesDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139Francisco J. CastanderInstitut d’Estudis Espacials de Catalunya/CSIC, Gran Capità 2-4, E-08034 Barcelona, SpainAndrew ConnollyDepartment of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260Istvan CsabaiDepartment of Physics of Complex Systems, Eötvös University, Pázmány Péter sétány 1, H-1518 Budapest, HungaryMamoru DoiInstitute of Astronomy, School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, JapanMasataka FukugitaInstitute for Cosmic Ray Research, University of Tokyo, Kashiwa 277-8582, JapanJoshua A. FriemanFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Karl GlazebrookDepartment of Physics and Astronomy, Johns Hopkins University, 3701 San Martin Drive, Baltimore, MD 21218James E. GunnPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544John S. HendryFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Gregory HennessyUnited States Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002Zeljko IvezićDepartment of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580Stephen KentFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Gillian R. KnappPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Huan LinFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Yeong‐Shang LohCenter for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80803Robert H. LuptonPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Bruce MargonSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Timothy A. McKayDepartment of Physics, University of Michigan, Ann Arbor, MI 48109-1120Avery MeiksinInstitute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UKJeffery A. MunnUnited States Naval Observatory, Flagstaff Station, P.O. Box 1149, Flagstaff, AZ 86002Adrian PopeDepartment of Physics and Astronomy, Johns Hopkins University, 3701 San Martin Drive, Baltimore, MD 21218Michael W. RichmondDepartment of Physics, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623-5603David SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, MS 50R-5032, Berkeley, CA 94720-8160Donald P. SchneiderDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802Kazuhiro ShimasakuDepartment of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanChristopher StoughtonFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Michael A. StraussPrinceton University Observatory, Peyton Hall, Princeton, NJ 08544Mark SubbaRaoAdler Planetarium, 1300 South Lake Shore Drive, Chicago, IL 60605Alexander S. SzalayDepartment of Physics and Astronomy, Johns Hopkins University, 3701 San Martin Drive, Baltimore, MD 21218Istvan SzapudiInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822Douglas L. TuckerFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Brian YannyFermilab National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510Donald G. YorkUniversity of Chicago, Astronomy and Astrophysics Center, 5640 South Ellis Avenue, Chicago, IL 60637

2005en

ABI

Аннотация

We present the large-scale correlation function measured from a spectroscopic sample of 46,748 luminous red galaxies from the Sloan Digital Sky Survey. The survey region covers 0.72 h^{-3} Gpc^3 over 3816 square degrees and 0.16<z<0.47, making it the best sample yet for the study of large-scale structure. We find a well-detected peak in the correlation function at 100h^{-1} Mpc separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter. This detection demonstrates the linear growth of structure by gravitational instability between z=1000 and the present and confirms a firm prediction of the standard cosmological theory. The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to z=0.35 and z=1089 to 4% fractional accuracy and the absolute distance to z=0.35 to 5% accuracy. From the overall shape of the correlation function, we measure the matter density Omega_mh^2 to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies. Independent of the constraints provided by the CMB acoustic scale, we find Omega_m = 0.273 +- 0.025 + 0.123 (1+w_0) + 0.137 Omega_K. Including the CMB acoustic scale, we find that the spatial curvature is Omega_K=-0.010+-0.009 if the dark energy is a cosmological constant. More generally, our results provide a measurement of cosmological distance, and hence an argument for dark energy, based on a geometric method with the same simple physics as the microwave background anisotropies. The standard cosmological model convincingly passes these new and robust tests of its fundamental properties.

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DOI: 10.1086/466512

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