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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift space distortions using the power spectrum multipoles

Research output: Contribution to journalArticle

  • Florian Beutler
  • Shun Saito
  • Hee Jong Seo
  • Jon Brinkmann
  • Kyle S. Dawson
  • Daniel J. Eisenstein
  • Andreu Font-Ribera
  • Shirley Ho
  • Cameron K. McBride
  • Francesco Montesano
  • Will J. Percival
  • Ashley J. Ross
  • Nic Ross
  • Lado Samushia
  • David J. Schlegel
  • Ariel G. Sánchez
  • Jeremy L. Tinker
  • Benjamin A. Weaver

Related Edinburgh Organisations

Original languageEnglish
Article numberstu1051
Pages (from-to)1065-1089
Number of pages25
JournalMonthly Notices of the Royal Astronomical Society
Issue number2
StatePublished - 2014


We analyse the anisotropic clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) CMASS Data Release 11 (DR11) sample, which consists of 690 827 galaxies in the redshift range 0.43 < z < 0.7 and has a sky coverage of 8498 deg2. We perform our analysis in Fourier space using a power spectrum estimator suggested by Yamamoto et al. We measure the multipole power spectra in a self-consistent manner for the first time in the sense that we provide a proper way to treat the survey window function and the integral constraint, without the commonly used assumption of an isotropic power spectrum and without the need to split the survey into subregions. The main cosmological signals exploited in our analysis are the baryon acoustic oscillations and the signal of redshift space distortions, both of which are distorted by the Alcock-Paczynski effect. Together, these signals allow us to constrain the distance ratio DV(zeff)/rs(zd) = 13.89 ± 0.18, the Alcock-Paczynski parameter FAP(zeff) = 0.679 ± 0.031 and the growth rate of structure f(zeff8(zeff) = 0.419 ± 0.044 at the effective redshift zeff = 0.57.We emphasize that our constraints are robust against possible systematic uncertainties. In order to ensure this, we perform a detailed systematics study against CMASS mock galaxy catalogues and N-body simulations. We find that such systematics will lead to 3.1 per cent uncertainty for fσ8 if we limit our fitting range to k = 0.01-0.20 h Mpc-1, where the statistical uncertainty is expected to be three times larger. We did not find significant systematic uncertainties for DV/rs or FAP. Combining our data set with Planck to test General Relativity (GR) through the simple γ -parametrization, where the growth rate is given by f (z) =ωγ m(z), reveals ã2σ tension between the data and the prediction by GR. The tension between our result and GR can be traced back to a tension in the clustering amplitude σ8 between CMASS and Planck.

    Research areas

  • Cosmological parameters, Cosmology: observations, Dark energy, Gravitation, Large-scale structure of universe, Surveys

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