TY - JOUR

T1 - The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey

T2 - single-probe measurements and the strong power of f(z)Sigma(8)(z) on constraining dark energy

AU - Chuang, Chia-Hsun

AU - Prada, Francisco

AU - Cuesta, Antonio J.

AU - Eisenstein, Daniel J.

AU - Kazin, Eyal

AU - Padmanabhan, Nikhil

AU - Sanchez, Ariel G.

AU - Xu, Xiaoying

AU - Beutler, Florian

AU - Manera, Marc

AU - Schlegel, David J.

AU - Schneider, Donald P.

AU - Weinberg, David H.

AU - Brinkmann, Jon

AU - Brownstein, Joel R.

AU - Thomas, Daniel

PY - 2013/8/21

Y1 - 2013/8/21

N2 - We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z)σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation bσ8(z). We obtain {H(0.57), DA(0.57), f (0.57)σ8(0.57), Ωmh2, bσ8(0.57)} = {87.6+6.7−6.8 kms−1 Mpc−1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008 -0.010 ,1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w = −0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.

AB - We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance DA(z), the normalized growth rate f (z)σ8(z), the physical matter density Ωmh2, and the biased amplitude of matter fluctuation bσ8(z). We obtain {H(0.57), DA(0.57), f (0.57)σ8(0.57), Ωmh2, bσ8(0.57)} = {87.6+6.7−6.8 kms−1 Mpc−1, 1396 ± 73 Mpc, 0.428 ± 0.066, 0.126+0.008 -0.010 ,1.19 ± 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)σ8(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w = −0.90 ± 0.11. Therefore, it is important to include f (z)σ8(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys.

KW - cosmological parameters

KW - cosmology: observations

KW - distance scale

KW - large-scale structure of Universe

U2 - 10.1093/mnras/stt988

DO - 10.1093/mnras/stt988

M3 - Article

SN - 0035-8711

VL - 433

SP - 3559

EP - 3571

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -