The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: testing deviations from Λ and general relativity using anisotropic clustering of galaxies

By L. Samushia, B. Reid, M. White, Will J. Percival, A. Cuesta, L. Lombriser, Marc Manera, Robert Nichol, D. Schneider, D. Bizyaev and 12 more. 2012

197 citations recorded by the source corpus.

We use the joint measurement of geometry and growth from anisotropic galaxy clustering in the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 9 (DR9) CMASS sample reported by Reid et al. to constrain dark energy (DE) properties and possible deviations from the general relativity (GR). Assuming GR and taking a prior on the linear matter power spectrum at high redshift from the cosmic microwave background (CMB), anisotropic clustering of the CMASS DR9 galaxies alone constrains Ωm = 0.308 ± 0.022 and 100Ωk = 5.9 ± 4.8 for w = −1, or w = −0.91 ± 0.12 for Ωk = 0. When combined with the full CMB likelihood, the addition of the anisotropic clustering measurements to the spherically averaged baryon acoustic oscillation location increases the constraining power on DE by a factor of 4 in a flat cold dark matter (CDM) cosmology with constant DE equation of state w (giving w = −0.87 ± 0.05). This impressive gain depends on our measurement of both the growth of structure and the Alcock–Paczynski effect, and is not realized when marginalizing over the amplitude of redshift-space distortions. Combining with both the CMB and Type Ia supernovae, we find Ωm = 0.281 ± 0.014 and 1000Ωk = −9.2 ± 5.0 for w = −1, or w0 = −1.13 ± 0.12 and wa = 0.65 ± 0.36 assuming Ωk = 0. Finally, when a ΛCDM background expansion is assumed, the combination of our estimate of the growth rate with previous growth measurements provides tight constraints on the parameters describing possible deviations from GR giving γ = 0.64 ± 0.05. For one-parameter extensions of the flat ΛCDM model, we find a ∼2σ preference either for w > −1 or slower growth than in GR. However, the data are fully consistent with the concordance model, and evidence for these additional parameters is weaker than 2σ.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/b238cc0f971745d2d4dd9192255e59f9b1d91a8d

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Citations in the corpus

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, methodology): “Using the fiducial values for σ 8(zeff) the bias obtained in our analysis is b1 = 2.040 ± 0.052, while Samushia et al. (2013b) find b1 = 2.096 ± 0.052.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, methodology): “…measurements based on data from the SDSS-III (Eisenstein et al. 2011) Baryon Oscillation Spectroscopic Survey (BOSS; Dawson et al. 2013), clearly illustrated their constraining power (Anderson et al. 2014a,b; Reid et al. 2012; Chuang et al. 2013; Samushia et al. 2013, 2014; Beutler et al. 2014).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “…measurements from earlier BOSS data releases, using a variety of technical approaches, include Reid et al. (2012, 2014); Tojeiro et al. (2012); Chuang et al. (2013a); Samushia et al. (2013, 2014); Sánchez et al. (2013, 2014); Beutler et al. (2014a); Gil-Marı́n et al. (2016b); Alam et al. (2015b).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “Independent constraints from other data sets have been obtained by, e.g., Nesseris & Perivolaropoulos (2008), di Porto & Amendola (2008), Samushia et al. (2013, 2014) and Beutler et al. (2014a).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring DA and H at z = 0.57 from the baryon acoustic peak in the data release 9 spectroscopic galaxy sample (2013, background): “This additional information has been studied in Reid et al. (2012), Samushia et al. (2013), and Tojeiro et al. (2012).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Measuring growth rate and geometry with anisotropic clustering (2013, methodology): “Our constraints on w differ significantly from the DR9 results presented in Samushia et al. (2013), where we detected up to 2σ preference for w > −1.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “…of f(z)σ 8(z) from CMB data (Planck) with our measurement (red square), other measurements from BOSS galaxy sample (blue triangle; Beutler et al. 2014; Samushia et al. 2014; Alam et al. 2015; Gil-Marin et al. 2015a) and the measurements compiled by Samushia et al. (2013) (black circles).”
Is there a "too big to fail" problem in the field? (2014, background): “Remarkably, sub-percent accuracy measurements of the cosmic microwave background and few percent measurements of the large scale distribution of galaxies have yielded no evidence for deviations from the “standard” cosmological model (Planck Collaboration et al. 2013; Samushia et al. 2013).”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, background): “Observations of RSDs provide an exciting opportunity to constrain models of modified gravity (Zhang et al. 2007; Reyes et al. 2010; Samushia et al. 2013).”
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 (2013, methodology): “These measurements have been complemented by analyses of the full shape of isotropic and anisotropic clustering measurements (Reid et al. 2012; Sánchez et al. 2012, 2013; Chuang et al. 2013a; Samushia et al. 2013a).”
MODEL-INDEPENDENT EVIDENCE FOR DARK ENERGY EVOLUTION FROM BARYON ACOUSTIC OSCILLATIONS (2014, unknown): “…z3) = 0.122 ± 0.012, (6) where z1 = 0, z2 = 0.57 , and z3 = 2.34, and the Hubble parameters at these redshifts are H (z = 0) = 70.6 ± 3.3 km s−1 Mpc−1 (Efstathiou 2014), H (z = 0.57) = 92.4 ± 4.5 km s−1 Mpc−1 (Samushia et al. 2013), and H (z = 2.34) = 222 ± 7 km s−1 Mpc−1 (Delubac et al. 2014).”
THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW AND EARLY DATA (2015, unknown): “BOSS Constraints on RSD and Modified Gravity Reid et al. (2012) and Samushia et al. (2013) presented the first measurements and cosmological interpretation of RSD in the BOSS DR9 galaxy sample.”
SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues (2015, methodology): “RSD were measured by Reid et al. (2012) and enhanced by knowledge of passive galaxy evolution in Tojeiro et al. (2012); the resulting GR tests were presented in Samushia et al. (2013).”
The DESI Experiment Part I: Science,Targeting, and Survey Design (2016, background): “1: Compilation of RSD-based fσ8 measurements from [89].”