Maqola

Baryon acoustic oscillations in the Ly<i>α</i>forest of BOSS quasars

N. G. BuscaAPC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, Paris, FranceT. DelubacCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceJ. RichCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceS. BaileyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAA. Font-RiberaInstitute of Theoretical Physics, University of Zurich, 8057 Zurich, SwitzerlandD. KirkbyDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USAJ.-M. Le GoffCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceM. M. PieriInstitute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UKA. SlosarBldg 510 Brookhaven National Laboratory, Upton, NY 11973, USAÉ. AubourgAPC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, Paris, FranceJ. E. BautistaAPC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, Paris, FranceD. BizyaevM. BlomqvistDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USAA. S. BoltonDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USAJ. BovyInstitute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USAH. BrewingtonA. BordeCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceJ. BrinkmannB. CarithersLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAR. A. C. CroftBruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, Pittsburgh, PA 15213, USAK. S. DawsonDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USAG. EbelkeD. J. EisensteinHarvard-Smithsonian Center for Astrophysics, Harvard University, 60 Garden St., Cambridge MA 02138, USAJ.-C. HamiltonAPC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, Paris, FranceS. HoBruce and Astrid McWilliams Center for Cosmology, Carnegie Mellon University, Pittsburgh, PA 15213, USAD. W. HoggCenter for Cosmology and Particle Physics, New York University, New York, NY 10003, USAK. HonscheidDepartment of Physics and Center for Cosmology and Astro-Particle Physics, Ohio State University, Columbus, OH 43210, USAK.-G. LeeMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, GermanyB. LundgrenE. MalanushenkoV. MalanushenkoD. MargalaDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USAC. MarastonInstitute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UKK. MehtaSteward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85121, USAJ. Miralda-EscudéInstitució Catalana de Recerca i Estudis Avançats, Barcelona, CataloniaA. D. MyersDepartment of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USAR. C. NicholInstitute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UKP. NoterdaemeUniversité Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis blvd. Arago, 75014 Paris, FranceM. D. OlmsteadDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USAD. OravetzN. Palanque-DelabrouilleCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceK. PanI. PârisDepartamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, ChileW. J. PercivalInstitute of Cosmology and Gravitation, Dennis Sciama Building, University of Portsmouth, Portsmouth, PO1 3FX, UKP. PetitjeanUniversité Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis blvd. Arago, 75014 Paris, FranceN. A. RoeLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAE. RollindeUniversité Paris 6 et CNRS, Institut d’Astrophysique de Paris, 98bis blvd. Arago, 75014 Paris, FranceN. P. RossLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAG. RossiCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceD. J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAD. P. SchneiderDepartment of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USAA. SheldenE. S. SheldonBldg 510 Brookhaven National Laboratory, Upton, NY 11973, USAA. SimmonsS. SneddenBldg 510 Brookhaven National Laboratory, Upton, NY 11973, USAJ. L. TinkerCenter for Cosmology and Particle Physics, New York University, New York, NY 10003, USAM. VielINAF, Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, ItalyB. A. WeaverCenter for Cosmology and Particle Physics, New York University, New York, NY 10003, USAD. H. WeinbergDepartment of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAM. WhiteLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAC. YècheCEA, Centre de Saclay, IRFU, 91191 Gif-sur-Yvette, FranceD. G. YorkDepartment of Astronomy and Astrophysics and the Enrico Fermi Institute, The University of Chicago, 5640 South Ellis Avenue, Chicago, Illinois, 60615, USA

2013en

ABI

Annotatsiya

We report a detection of the baryon acoustic oscillation (BAO) feature in the three-dimensional correlation function of the transmitted flux fraction in the Lyα forest of high-redshift quasars. The study uses 48 640 quasars in the redshift range 2.1 ≤ z ≤ 3.5 from the Baryon Oscillation Spectroscopic Survey (BOSS) of the third generation of the Sloan Digital Sky Survey (SDSS-III). At a mean redshift z = 2.3, we measure the monopole and quadrupole components of the correlation function for separations in the range 20 h-1 Mpc < r < 200 h-1 Mpc. A peak in the correlation function is seen at a separation equal to (1.01 ± 0.03) times the distance expected for the BAO peak within a concordance ΛCDM cosmology. This first detection of the BAO peak at high redshift, when the universe was strongly matter dominated, results in constraints on the angular diameter distance DA and the expansion rate H at z = 2.3 that, combined with priors on H0 and the baryon density, require the existence of dark energy. Combined with constraints derived from cosmic microwave background observations, this result implies H(z = 2.3) = (224 ± 8) km s-1 Mpc-1, indicating that the time derivative of the cosmological scale parameter ȧ = H(z = 2.3)/(1 + z) is significantly greater than that measured with BAO at z ~ 0.5. This demonstrates that the expansion was decelerating in the range 0.7 < z < 2.3, as expected from the matter domination during this epoch. Combined with measurements of H0, one sees the pattern of deceleration followed by acceleration characteristic of a dark-energy dominated universe.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1051/0004-6361/201220724

Iqtiboslar va manbalar

10 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar