The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring growth rate and geometry with anisotropic clustering

Samushia, Lado; Reid, Beth A.; White, Martin; Percival, Will J.; Cuesta, Antonio J.; Zhao, Gong-Bo; Ross, Ashley J.; Manera, Marc; Aubourg, Éric; Beutler, Florian; Brinkmann, Jon; Brownstein, Joel R.; Dawson, Kyle S.; Eisenstein, Daniel J.; Ho, Shirley; Honscheid, Klaus; Maraston, Claudia; Montesano, Francesco; Nichol, Robert C.; Roe, Natalie A.; Ross, Nicholas P.; Sánchez, Ariel G.; Schlegel, David J.; Schneider, Donald P.; Streblyanska, Alina; Thomas, Daniel; Tinker, Jeremy L.; Wake, David A.; Weaver, Benjamin A. and Zehavi, Idit (2014). The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring growth rate and geometry with anisotropic clustering. Monthly Notices of the Royal Astronomical Society, 439(4) pp. 3504–3519.

DOI: https://doi.org/10.1093/mnras/stu197

Abstract

We use the observed anisotropic clustering of galaxies in the Baryon Oscillation Spectroscopic Survey Data Release 11 CMASS sample to measure the linear growth rate of structure, the Hubble expansion rate and the comoving distance scale. Our sample covers 8498 deg² and encloses an effective volume of 6 Gpc³ at an effective redshift of z̄=0.57. We find fσ₈ = 0.441 ± 0.044, H = 93.1 ± 3.0 km s^-1 Mpc^-1 and D_A = 1380 ± 23 Mpc when fitting the growth and expansion rate simultaneously. When we fix the background expansion to the one predicted by spatially flat Λ cold dark matter (ΛCDM) model in agreement with recent Planck results, we find fσ₈ = 0.447 ± 0.028 (6 per cent accuracy). While our measurements are generally consistent with the predictions of ΛCDM and general relativity, they mildly favour models in which the strength of gravitational interactions is weaker than what is predicted by general relativity. Combining our measurements with recent cosmic microwave background data results in tight constraints on basic cosmological parameters and deviations from the standard cosmological model. Separately varying these parameters, we find w = −0.983 ± 0.075 (8 per cent accuracy) and γ = 0.69 ± 0.11 (16 per cent accuracy) for the effective equation of state of dark energy and the growth rate index, respectively. Both constraints are in good agreement with the standard model values of w = −1 and γ = 0.554.

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