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

By F. Beutler, S. Saito, H. Seo, J. Brinkmann, K. Dawson, Daniel J. Eisenstein, A. Font-Ribera, Shirley Ho, Cameron McBride, F. Montesano and 8 more. 2013

276 citations recorded by the source corpus.

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)σ_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 fσ_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 F_AP. Combining our data set with Planck to test General Relativity (GR) through the simple γ-parametrization, where the growth rate is given by $f(z) = \Omega ^{\gamma }_{\rm m}(z)$, reveals a ∼2σ 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 σ_8 between CMASS and Planck.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b85e23adb1897fe7a755992fd080c8268848a9b8

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies (2016, methodology): “We assume an Eulerian non-linear and non-local bias model, as proposed by McDonald & Roy (2009) and used in previous analysis of the power spectrum and bispectrum of BOSS data (Beutler et al. 2014; Gil-Maŕın et al. 2015a, 2016a).”
THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III (2015, methodology): “…BAO in the cross-correlation between the Lyman-α forest and the quasars (Font-Ribera et al. 2014), an updated upper bound to the sum of neutrino masses (Beutler et al. 2014a), a summary BAO galaxy clustering analysis paper (Anderson et al. 2014b), and a joint cosmology analysis paper…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, methodology): “(23) The closest redshift-space model in the literature to ours (Taruya et al. 2010; Beutler et al. 2014) also starts from equation (15).”
The cosmological analysis of the SDSS/BOSS data from the Effective Field Theory of Large-Scale Structure (2019, background): “In fact, these parameters were never measured individually, and in such an 24See also [92] for a different numerical implementation.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “Besides the covariance matrix, which is derived from 2045 MD-Patchy mock catalogues, this analysis depends on a framework for the wedge window function, which was developed based on the recipe for the power spectrum multipoles of Beutler et al. (2014a).”
Cosmic Discordance: Are Planck CMB and CFHTLenS weak lensing measurements out of tune? (2014, methodology): “Beutler et al. (2014a) already noted a ≈ 1σ shift in the constraint on σ8 from using the newer implementation of 2 http://www.hep.anl.gov/cosmology/CosmicEmu/emu.html Halofit.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Constraining modified gravity (2016, result): “We can improve upon previous studies, i.e. Beutler et al. (2014) , by 30-40%.”
THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW AND EARLY DATA (2015, unknown): “Estimates from the clustering of BOSS galaxies have already shown the potential in spectroscopic surveys to constrain the neutrino mass (e.g. Zhao et al. 2013; Beutler et al. 2014a).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: a tomographic measurement of cosmic structure growth and expansion rate based on optimal redshift weights (2018, methodology): “We use the extended TNS model (Taruya, Nishimichi & Saito 2010) used in Beutler et al. (2014, 2017) and Alam et al. (2017) as a template of the two-dimensional power spectrum at a given redshift z, Pg(k, μ, z) = DFoG (k, μ, z) [ Pg,δδ(k, z) +2f (z)μ2Pg,δθ (k, z) + f 2(z)μ4Pθθ (k, z) +A(k, μ, z) + B…”
SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues (2015, methodology): “As for DR9, the results were extensively used, further testing the catalogues: RSD measurements have been made in a number of different ways (Beutler et al. 2014a; Samushia et al. 2014; Sanchez et al. 2014; Chuang et al. 2013), the bispectrum calculated and analysed (Gil-Marin et al. 2015a,b), and…”
Testing Inflation with Large Scale Structure: Connecting Hopes with Reality (2014, background): “The survey mask is difficult to account for already in the power spectrum already [138] and might be even more difficult in the bispectrum.”
KiDS-450 + 2dFLenS: Cosmological parameter constraints from weak gravitational lensing tomography and overlapping redshift-space galaxy clustering (2017, methodology): “Our conclusions are qualitatively unchanged by different implementations of the shot noise nuisance parameter (Beutler et al. 2014).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…(2016) D ow nloaded from https://academ ic.oup.com /m nras/article-abstract/461/4/3781/2608598 by guest on 15 M arch 2020 Sanchez et al. 2013a; Beutler et al. 2014; Samushia et al. 2014; Tojeiro et al. 2014; Wang 2014; Alam et al. 2015; Gil-Marin et al. 2015a,b; Cuesta et al. 2016) In Figs…”
Planck2015 results (2015, unknown): “The Beutler et al. (2014a) analysis is performed in Fourier space and shows a small bias in fσ8 compared to numerical simulations when fitting over the wavenumber range 0.01−0.20 h Mpc−1.”