Interpreting large-scale redshift-space distortion measurements

By L. Samushia, Will J. Percival, A. Raccanelli. 2011

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The simplest theory describing large-scale redshift-space distortions (RSD), based on linear theory and distant galaxies, depends on the growth of cosmological structure, suggesting that strong tests of general relativity can be constructed from galaxy surveys. As data sets become larger and the expected constraints more precise, the extent to which the RSD follow the simple theory needs to be assessed in order that we do not introduce systematic errors into the tests by introducing inaccurate simplifying assumptions. We study the impact of the sample geometry, non-linear processes and biases induced by our lack of understanding of the radial galaxy distribution on RSD measurements. Using Large Suite of Dark Matter Simulations of the Sloan Digital Sky Survey II (SDSS-II) luminous red galaxy data, these effects are shown to be important at the level of 20 per cent. Including them, we can accurately model the recovered clustering in these mock catalogues on scales 30–200 h−1 Mpc. Applying this analysis to robustly measure parameters describing the growth history of the Universe from the SDSS-II data gives f(z= 0.25)σ8(z= 0.25) = 0.3512 ± 0.0583 and f(z= 0.37)σ8(z= 0.37) = 0.4602 ± 0.0378 when no prior is imposed on the growth rate, and the background geometry is assumed to follow a Λ cold dark matter (ΛCDM) model with the Wilkinson Microwave Anisotropy Probe (WMAP)+Type Ia supernova priors. The standard WMAP constrained ΛCDM model with general relativity predicts f(z= 0.25)σ8(z= 0.25) = 0.4260 ± 0.0141 and f(z= 0.37)σ8(z= 0.37) = 0.4367 ± 0.0136, which is fully consistent with these measurements.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5b71db59fca1901c841539b117c5ed874de5e1c2

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Citations in the corpus

Galaxy And Mass Assembly (GAMA): improved cosmic growth measurements using multiple tracers of large-scale structure (2013, methodology): “These measurements were taken from 6dFGS (z = 0.067; Beutler et al. 2012), 2dFGRS (z = 0.17; Hawkins et al. 2003), the SDSS Luminous Red Galaxy sample (z = 0.25 and 0.37; Samushia et al. 2012) and the WiggleZ Survey (z = 0.22 and 0.41; Blake et al. 2011).”
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 (2012, methodology): “Most were made by assuming a fixed fiducial cosmological model, while Samushia et al. (2012) and Reid etal.”
The VIMOS Public Extragalactic Redshift Survey (VIPERS) - Galaxy clustering and redshift-space distortions at z ≃ 0.8 in the first data release (2013, methodology): “…as a test of gravity theories was the analysis of the VVDS survey by Guzzo et al. (2008), and subsequent work especially by the SDSS LRG (Samushia et al. 2012), WiggleZ (Blake et al. 2012; Contreras et al. 2013), 6dFGS (Beutler et al. 2012) and BOSS (Reid et al. 2012) surveys has…”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “…the studies of the 6dFGS (Beutler et al. 2012), the SDSS main galaxies (Howlett et al. 2015), the 2dFGRS (Song & Percival 2009), the SDSS LRG (Samushia et al. 2012), the BOSS LOWZ (Chuang et al. 2013), the BOSS CMASS (Reid et al. 2012), WiggleZ (Blake et al. 2011), VVDS (Guzzo et al. 2008)…”
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): “Within the luminous red galaxy sample in SDSS-II DR7, Samushia et al. (2012) reported growth of structure measurements in two redshift bins, finding f(z = 0.25)σ 8(z = 0.25) = 0.351 ± 0.058 and f(z = 0.37)σ 8(z = 0.37) = 0.460 ± 0.038.”
Numerical simulations of the dark universe: State of the art and the next decade (2012, background): “simulations have highlighted the pitfalls of this approach and the systematic error that it would introduce for future surveys [168, 193, 197, 198].”
Holographic dark energy (2016, methodology): “Now this quantity is often used to constrain DE together with the BAO information [137, 138].”
LATE-TIME COSMOLOGY WITH 21 cm INTENSITY MAPPING EXPERIMENTS (2014, methodology): “…have used a Lorentzian instead of an exponential, or a slightly more complex exponential term that models non-linear smoothing of the BAO as well (Samushia et al. 2012). s » 4 and 10NL Mpc (e.g., Li et al. 2007; Reid & White 2011; Reid et al. 2012; Contreras et al. 2013); for our fiducial model,…”
Evolution of the f σ 8 tension with the Planck 15 / Λ CDM determination and implications for modified gravity theories (2018, neutral): “0586 [80] 9 December 2011 10 WiggleZ 0.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of f(z)σ8(z) on constraining dark energy (2013, methodology): “Similar analysis have been also applied on the SDSS-III BOSS CMASS sample and obtained the most precise measurements to date (Anderson et al. 2012; Manera et al. 2013; Nuza et al. 2012; Reid et al. 2012; Samushia et al. 2012; Tojeiro et al. 2012).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Constraining modified gravity (2016, methodology): “Similarly, due to the slight overlap with BOSS, we do not include the WiggleZ (Blake et al. 2011) and Data Release 7 LRG (Samushia et al. 2012) measurements, since both have much less precision than DR12.”
Simultaneous constraints on the growth of structure and cosmic expansion from the multipole power spectra of the SDSS DR7 LRG sample (2013, methodology): “Secondly, a couple of previous works addressed the anisotropic signal of LRGs via the correlation function (Samushia et al. 2012; Xu et al. 2013), but they did not consider a simultaneous constraint on f , DA and H via the AP effect and RSDs.”
Observational probes of cosmic acceleration (2012, methodology): “…analyses include the measurement of Guzzo et al. (2008) from the VIMOS-VLT Deep Survey (VVDS), f(z) = 0.91 ± 0.36 at z ≈ 0.8, the measurement of Samushia et al. (2012) from SDSS DR7, obtaining ∼ 10% constraints on f(z)σ8(z) at z = 0.25 and z = 0.37, the measurement of Blake et al. (2011a)…”