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

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 deg(2). 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 D-V(z(eff))/r(s)(z(d)) = 13.89 +/- 0.18, the Alcock-Paczynski parameter F-AP(z(eff)) = 0.679 +/- 0.031 and the growth rate of structure f (z(eff))sigma(8)(z(eff)) = 0.419 +/- 0.044 at the effective redshift z(eff) = 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 f sigma(8) 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 D-V/r(s) or FAP. Combining our data set with Planck to test General Relativity (GR) through the simple gamma-parametrization, where the growth rate is given by f (z) = Omega(gamma)(m)(z), reveals a similar to 2 sigma 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 sigma(8) between CMASS and Planck.