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The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space

Florian BeutlerInstitute of Cosmology and Gravitation, Dennis Sciama Building, Univer-sity of Portsmouth, Portsmouth PO1 3FX, UKHee‐Jong SeoDepartment of Physics and Astronomy, Ohio University, 251B Clippinger Labs, Athens, OH 45701, USAA.J. RossDepartment of Physics, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USAPatrick McDonaldLawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USAShun SaitoKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, JapanA. BoltonDepartment of Physics and Astronomy, University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAJoel R. BrownsteinDepartment of Physics and Astronomy, University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USAChia-Hsun ChuangInstituto de Fsica Terica (UAM/CSIC), Universidad Autnoma de Madrid, Cantoblanco, E-28049 Madrid, SpainAntonio J. CuestaInstitut de Cincies del Cosmos (ICCUB), Universitat de Barcelona (IEEC-UB), Mart i Franqus 1, E-08028 Barcelona, SpainDaniel J. EisensteinHarvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USAAndreu Font-RiberaKavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, JapanJan Niklas GriebMax-Planck-Institut fr extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, GermanyNick HandDepartment of Astronomy, University of California, Berkeley, CA 94720, USAFrancisco-Shu KitauraLeibniz-Institut fr Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, GermanyChirag ModiDepartment of Physics, University of California, Berkeley, CA 94720, USARobert C. NicholInstitute of Cosmology and Gravitation, Dennis Sciama Building, Univer-sity of Portsmouth, Portsmouth PO1 3FX, UKWill J. PercivalInstitute of Cosmology and Gravitation, Dennis Sciama Building, Univer-sity of Portsmouth, Portsmouth PO1 3FX, UKFrancisco PradaCampus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, SpainSergio Rodríguez-TorresCampus of International Excellence UAM+CSIC, Cantoblanco, E-28049 Madrid, SpainNatalie A. RoeLawrence Berkeley National Lab, 1 Cyclotron Rd, Berkeley, CA 94720, USANicholas P. RossInstitute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh EH9 3HJ, UKSalvador Salazar-AlbornozMax-Planck-Institut fr extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, GermanyAriel G. SánchezMax-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstr., D-85741 Garching, GermanyDonald P. SchneiderDepartment of Astronomy and Astrophysics, The Pennsylvania State Uni-versity, University Park, PA 16802, USAAnže SlosarBrookhaven National Laboratory, Upton, NY 11973, USAJeremy L. TinkerCenter for Cosmology and Particle Physics, Department of Physics, New York University, 4 Washington Place, New York, NY 10003, USARita TojeiroSchool of Physics and Astronomy, University of St. Andrews, St Andrews, Fife KY16 9SS, UKM. Vargas-MagañaInstituto de Fisica, Universidad Nacional Autonoma de Mexico, Apdo. Postal 20-364, MexicoJ. Alberto VázquezBrookhaven National Laboratory, Upton, NY 11973, USA

2016en

ABI

Annotatsiya

We analyse the baryon acoustic oscillation (BAO) signal of the final Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our analysis is performed in the Fourier space, using the power spectrum monopole and quadrupole. The data set includes 1198 006 galaxies over the redshift range 0.2 < z < 0.75. We divide this data set into three (overlapping) redshift bins with the effective redshifts z eff = 0.38, 0.51 and 0.61. We demonstrate the reliability of our analysis pipeline using N-body simulations as well as 1000 MultiDark-Patchy mock catalogues that mimic the BOSS-DR12 target selection. We apply density field reconstruction to enhance the BAO signal-to-noise ratio. By including the power spectrum quadrupole we can separate the line of sight and angular modes, which allows us to constrain the angular diameter distance D A (z) and the Hubble parameter H(z) separately. We obtain two independent 1.6 and 1.5 per cent constraints on D A (z) and 2.9 and 2.3 per cent constraints on H(z) for the low (z eff = 0.38) and high (z eff = 0.61) redshift bin, respectively. We obtain two independent 1 and 0.9 per cent constraints on the angular averaged distance D V (z), when ignoring the Alcock-Paczynski effect. The detection significance of the BAO signal is of the order of 8 (post-reconstruction) for each of the three redshift bins. Our results are in good agreement with the Planck prediction within cold dark matter. This paper is part of a set that analyses the final galaxy clustering data set from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. to produce the final cosmological constraints from BOSS.

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DOI: 10.1093/mnras/stw2373

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