Статья

Measurement of baryon acoustic oscillation correlations at<i>z</i> = 2.3 with SDSS DR12 Ly<i>α</i>-Forests

Julian BautistaDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USANicolás G. BuscaAPC, Université Paris Diderot-Paris 7, CNRS/IN2P3, CEA, Observatoire de Paris, 10 rue A. Domon & L. Duquet, 75013 Paris, FranceJ. GuyLPNHE, CNRS/IN2P3, Université Pierre et Marie Curie Paris 6, Université Denis Diderot Paris 7, 4 place Jussieu, 75252 Paris CEDEX, FranceJames RichIRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, FranceMichael BlomqvistAix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, FranceHélion du Mas des BourbouxIRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, FranceMatthew M. PieriAix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, FranceAndreu Font-RiberaLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAS. BaileyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USATimothée DelubacLaboratoire d'Astrophysique, École Polytechnique Fedérale de Lausanne, 1015 Lausanne, SwitzerlandD. KirkbyDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USAJean-Marc Le GoffIRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, FranceDaniel MargalaDepartment of Physics and Astronomy, University of California, Irvine, CA 92697, USAAnže SlosarBrookhaven National Laboratory, 2 Center Road, Upton, NY 11973, USAJ. Alberto VázquezBrookhaven National Laboratory, 2 Center Road, Upton, NY 11973, USAJoel R. BrownsteinDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USAKyle DawsonDepartment of Physics and Astronomy, University of Utah, 115 S 1400 E, Salt Lake City, UT 84112, USADaniel J. EisensteinHarvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USAJordi Miralda‐EscudéInstitució Catalana de Recerca i Estudis Avançats, 08010 Barcelona, Catalonia, SpainP. NoterdaemeUniversité Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, FranceN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, 91191 Gif-sur-Yvette, FranceIsabelle PârisAix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, FrancePatrick PetitjeanUniversité Paris 6 et CNRS, Institut d'Astrophysique de Paris, 98bis boulevard Arago, 75014 Paris, FranceNicholas P. RossInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh, EH9 3HJ, UKDonald P. SchneiderInstitute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USADavid H. WeinbergDepartment of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAChristophe YècheLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA

2017en

ABI

Аннотация

Here, we use flux-transmission correlations in Ly alpha forests to measure the imprint of baryon acoustic oscillations (BAO). The study uses spectra of 157,783 quasars in the redshift range 2.1 <= z <= 3.5 from the Sloan Digital Sky Survey (SDSS) Data Release 12 (DR12). Besides the statistical improvements on our previous studies using SDSS DR9 and DR11, we have implemented numerous improvements in the analysis procedure, allowing us to construct a physical model of the correlation function and to investigate potential systematic errors in the determination of the BAO peak position. The Hubble distance, D-H = c/H(z), relative to the sound horizon is D-H(z = 2.33)/r(d) = 9.07 +/- 0.31. The best-determined combination of comoving angular-diameter distance, D-M, and the Hubble distance is found to be (DHDM0.3)-D-0.7/r(d) = 13.94 +/- 0.35. This value is 1.028 +/- 0.026 times the prediction of the flat-Lambda CDM model consistent with the cosmic microwave background (CMB) anisotropy spectrum. The errors include marginalization over the effects of unidentified high-density absorption systems and fluctuations in ultraviolet ionizing radiation. Independently of the CMB measurements, the combination of our results and other BAO observations determine the open-Lambda CDM density parameters to be Omega(M) = 0.296 +/- 0.029, Omega(Lambda) = 0.699 +/- 0.100 and Omega(k) = -0.002 +/- 0.119.

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Идентификаторы

DOI: 10.1051/0004-6361/201730533

Цитирования и источники

Цитирований: 4Использованных источников: 0

Показатели — AkademScholar