Skip to content

The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample

Research output: Contribution to journalArticle

  • Shadab Alam
  • Metin Ata
  • Stephen Bailey
  • Dmitry Bizyaev
  • Jonathan A. Blazek
  • Adam S. Bolton
  • Joel R. Brownstein
  • Angela Burden
  • Chia-Hsun Chuang
  • Johan Comparat
  • Antonio J. Cuesta
  • Kyle S. Dawson
  • Daniel J. Eisenstein
  • Stephanie Escoffier
  • Héctor Gil-Marín
  • Jan Niklas Grieb
  • Nick Hand
  • Shirley Ho
  • Karen Kinemuchi
  • David Kirkby
  • Francisco Kitaura
  • Elena Malanushenko
  • Viktor Malanushenko
  • Cameron K. McBride
  • Matthew D. Olmstead
  • Daniel Oravetz
  • Nikhil Padmanabhan
  • Nathalie Palanque-Delabrouille
  • Kaike Pan
  • Marcos Pellejero-Ibanez
  • Will J. Percival
  • Patrick Petitjean
  • Francisco Prada
  • Adrian M. Price-Whelan
  • Beth A. Reid
  • Sergio A. Rodríguez-Torres
  • Natalie A. Roe
  • Nicholas P. Ross
  • Graziano Rossi
  • Jose Alberto Rubiño-Martín
  • Ariel G. Sánchez
  • Shun Saito
  • Salvador Salazar-Albornoz
  • Siddharth Satpathy
  • Claudia G. Scóccola
  • David J. Schlegel
  • Donald P. Schneider
  • Hee-Jong Seo
  • Audrey Simmons
  • Anže Slosar
  • Michael A. Strauss
  • Molly E. C. Swanson
  • Jeremy L. Tinker
  • Rita Tojeiro
  • Mariana Vargas Magaña
  • Jose Alberto Vazquez
  • Licia Verde
  • David A. Wake
  • Yuting Wang
  • David H. Weinberg
  • Martin White
  • W. Michael Wood-Vasey
  • Christophe Yèche
  • Idit Zehavi
  • Zhongxu Zhai
  • Gong-Bo Zhao
We present cosmological results from the final galaxy clustering data set of the Baryon Oscillation Spectroscopic Survey, part of the Sloan Digital Sky Survey III. Our combined galaxy sample comprises 1.2 million massive galaxies over an effective area of 9329 deg2 and volume of 18.7 Gpc3, divided into three partially overlapping redshift slices centred at effective redshifts 0.38, 0.51 and 0.61. We measure the angular diameter distance DM and Hubble parameter H from the baryon acoustic oscillation (BAO) method, in combination with a cosmic microwave background prior on the sound horizon scale, after applying reconstruction to reduce non-linear effects on the BAO feature. Using the anisotropic clustering of the pre-reconstruction density field, we measure the product DMH from the Alcock–Paczynski (AP) effect and the growth of structure, quantified by fσ8(z), from redshift-space distortions (RSD). We combine individual measurements presented in seven companion papers into a set of consensus values and likelihoods, obtaining constraints that are tighter and more robust than those from any one method; in particular, the AP measurement from sub-BAO scales sharpens constraints from post-reconstruction BAOs by breaking degeneracy between DM and H. Combined with Planck 2016 cosmic microwave background measurements, our distance scale measurements simultaneously imply curvature ΩK = 0.0003 ± 0.0026 and a dark energy equation-of-state parameter w = −1.01 ± 0.06, in strong affirmation of the spatially flat cold dark matter (CDM) model with a cosmological constant (ΛCDM). Our RSD measurements of fσ8, at 6 per cent precision, are similarly consistent with this model. When combined with supernova Ia data, we find H0 = 67.3 ± 1.0 km s−1 Mpc−1 even for our most general dark energy model, in tension with some direct measurements. Adding extra relativistic species as a degree of freedom loosens the constraint only slightly, to H0 = 67.8 ± 1.2 km s−1 Mpc−1. Assuming flat ΛCDM, we find Ωm = 0.310 ± 0.005 and H0 = 67.6 ± 0.5 km s−1 Mpc−1, and we find a 95 per cent upper limit of 0.16 eV c−2 on the neutrino mass sum.
Original languageEnglish
Pages (from-to)2617-2652
JournalMonthly Notices of the Royal Astronomical Society
Volume470
Issue number3
Early online date28 Mar 2017
DOIs
Publication statusPublished - Sep 2017

Documents

  • cosmological analysis of the DR12 galaxy sample

    Rights statement: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

    Final published version, 7.54 MB, PDF document

Related information

Relations Get citation (various referencing formats)

ID: 5522624