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The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Towards a computationally efficient analysis without informative priors

Research output: Contribution to journalArticle

  • Marcos Pellejero-Ibanez
  • Chuang Chia-Hsun Chuang
  • J. A. Rubiño-Martín
  • Antonio J. Cuesta
  • Yuting Wang
  • Sergio Rodríguez-Torres
  • Francisco Prada
  • Anže Slosar
  • Jose A. Vazquez
  • Shadab Alam
  • Daniel J. Eisenstein
  • Jan Niklas Grieb
  • Shirley Ho
  • Francisco Shu Kitaura
  • Graziano Rossi
  • Salvador Salazar-Albornoz
  • Ariel G. Sánchez
  • Siddharth Satpathy
  • Seo Hee-Jong Seo
  • Jeremy L. Tinker
  • Rita Tojeiro
  • Mariana Vargas-Magaña
  • Joel R. Brownstein
  • Matthew D. Olmstead

We develop a new computationally efficient methodology called double-probe analysis with the aim of minimizing informative priors (those coming from extra probes) in the estimation of cosmological parameters. Using our new methodology, we extract the dark energy model-independent cosmological constraints from the joint data sets of the Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample and Planck cosmic microwave background (CMB) measurements. We measure the mean values and covariance matrix of {R, la, Ωbh2, ns, log(As), Ωk, H(z), DA(z), f(z8(z)}, which give an efficient summary of the Planck data and two-point statistics from the BOSS galaxy sample. The CMB shift parameters are R=ΩmH20√r(z∗) and la = πr(z*)/rs(z*), where z* is the redshift at the last scattering surface, and r(z*) and rs(z*) denote our comoving distance to the z* and sound horizon at z*, respectively; Ωb is the baryon fraction at z = 0. This approximate methodology guarantees that we will not need to put informative priors on the cosmological parameters that galaxy clustering is unable to constrain, i.e. Ωbh2 and ns. The main advantage is that the computational time required for extracting these parameters is decreased by a factor of 60 with respect to exact full-likelihood analyses. The results obtained show no tension with the flat Λ cold dark matter (ΛCDM) cosmological paradigm. By comparing with the full-likelihood exact analysis with fixed dark energy models, on one hand we demonstrate that the double-probe method provides robust cosmological parameter constraints that can be conveniently used to study dark energy models, and on the other hand we provide a reliable set of measurements assuming dark energy models to be used, for example, in distance estimations. We extend our study to measure the sum of the neutrino mass using different methodologies, including double-probe analysis (introduced in this study), full-likelihood analysis and single-probe analysis. From full-likelihood analysis, we obtain Σmν < 0.12 (68 per cent), assuming ΛCDM and Σmν < 0.20 (68 per cent) assuming owCDM. We also find that there is degeneracy between observational systematics and neutrino masses, which suggests that one should take great care when estimating these parameters in the case of not having control over the systematics of a given sample.

Original languageEnglish
Pages (from-to)4116-4133
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume468
Issue number4
Early online date28 Mar 2017
DOIs
StatePublished - 11 Jul 2017

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  • 10.1093mnrasstx

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

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