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Open Access Publications from the University of California

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the full shape of the clustering wedges in the data release 10 and 11 galaxy samples

  • Author(s): Sánchez, AG
  • Montesano, F
  • Kazin, EA
  • Aubourg, E
  • Beutler, F
  • Brinkmann, J
  • Brownstein, JR
  • Cuesta, AJ
  • Dawson, KS
  • Eisenstein, DJ
  • Ho, S
  • Honscheid, K
  • Manera, M
  • Maraston, C
  • Mcbride, CK
  • Percival, WJ
  • Ross, AJ
  • Samushia, L
  • Schlegel, DJ
  • Schneider, DP
  • Skibba, R
  • Thomas, D
  • Tinker, JL
  • Tojeiro, R
  • Wake, DA
  • Weaver, BA
  • White, M
  • Zehavi, I
  • et al.

We explore the cosmological implications of the angle-averaged correlation function, ξ(s), and the clustering wedges, ξ⊥(s) and ξ∥(s), of the LOWZ and CMASS galaxy samples from Data Releases 10 and 11 of the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey. Our results show no significant evidence for a deviation from the standard Λ cold dark matter model. The combination of the information from our clustering measurements with recent data from the cosmic microwave background is sufficient to constrain the curvature of the Universe to Ωk= 0.0010 ± 0.0029, the total neutrino mass to ∑mν< 0.23 eV (95 per cent confidence level), the effective number of relativistic species to Neff= 3.31 ± 0.27 and the dark energy equation of state to wDE= -1.051 ± 0.076. These limits are further improved by adding information from Type Ia supernovae and baryon acoustic oscillations from other samples. In particular, this data set combination is completely consistent with a time-independent dark energy equation of state, in which case we find wDE= -1.024 ± 0.052. We explore the constraints on the growth rate of cosmic structures assuming f(z) = Ωm(z)γand obtain γ = 0.69 ± 0.15, consistent with the predictions of general relativity of γ = 0.55. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.

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