Cosmological constraints from the SDSS luminous red galaxies

By Max Tegmark, Daniel J. Eisenstein, M. Strauss, D. Weinberg, M. Blanton, Joshua A. Frieman, M. Fukugita, James E. Gunn, A. Hamilton, G. Knapp and 57 more. 2006

1,206 citations recorded by the source corpus.

We measure the large-scale real-space power spectrum P(k) using luminous red galaxies (LRGs) in the Sloan Digital Sky Survey (SDSS) and use this measurement to sharpen constraints on cosmological parameters from the Wilkinson Microwave Anisotropy Probe (WMAP). We employ a matrix-based power spectrum estimation method using Pseudo-Karhunen-Loeve eigenmodes, producing uncorrelated minimum-variance measurements in 20 k-bands of both the clustering power and its anisotropy due to redshift-space distortions, with narrow and well-behaved window functions in the range 0.01h/Mpc 0.1h/Mpc and associated nonlinear complications, yet agree well with more aggressive published analyses where nonlinear modeling is crucial.

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Citations in the corpus

Cores in warm dark matter haloes: a Catch 22 problem (2012, result): “It is in excellent agreement with recent observations, such as measurements of the cosmic microwave background and large scale surveys (Tegmark et al. 2006; Komatsu et al. 2011).”
Measuring the cosmological parameters with the Ep,i–Eiso correlation of gamma-ray bursts (2008, background): “…Perlmutter et al. 1998; Perlmutter et al. 1999; Riess et al. 1998; Riess et al. 2004; Astier et al. 2006), Baryon Acoustic Oscillations (BAO) (e.g., Eisenstein et al. 2005; Tegmark et al. 2006; Percival et al. 2007), galaxy clusters (e.g., Rosati, Borgani & Norman 2002; Voit 2005).”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, background): “…are constraints from (baryon acoustic oscillations in) the galaxy power spectrum (Percival et al. 2001; Cole et al. 2005; Eisenstein et al. 2005; Tegmark et al. 2006; Hütsi 2006; Percival et al. 2007a,b,c; Padmanabhan et al. 2007; Gaztanaga, Cabré & Hui 2009; Percival et al. 2010; Blake et…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, background): “In the last decade, galaxy redshift surveys became large enough to test this prediction (Peacock et al. 2001; Hawkins et al. 2003; Tegmark et al. 2006; Guzzo et al. 2008; Yamamoto, Sato & Huetsi 2008; Blake et al. 2011a; Beutler et al. 2012; Reid et al. 2012; Chuang et al. 2013a; Nishimichi & Oka…”
Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample (2009, background): “Tegmark et al. (2006) analysed the SDSS Data Release 4 (DR4; AdelmanMcCarthy et al. 2006) luminous red galaxy (LRG) sample.”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “RSD has been analyzed for various redshift surveys (e.g.,Davis& Peebles 1983; Fisher et al. 1994; Peacock et al. 2001; Zehavi et al. 2002; Hawkins et al. 2003; Percival et al. 2004; Tegmark et al. 2004; daÂngela et al. 2005; Tegmark et al. 2006; Ross et al. 2007; Okumura et al. 2008).”
Massive neutrinos and the non‐linear matter power spectrum (2011, unknown): “0.6 eV (Elgaroy et al. 2002; Seljak et al. 2006; Tegmark et al. 2006; Gratton et al. 2008; Mantz et al. 2010; Thomas et al. 2010; Reid et al. 2010).”
Cosmological parameters from the BOSS galaxy power spectrum (2019, unknown): “[92–94].”
A QUANTITATIVE EXPLANATION OF THE OBSERVED POPULATION OF MILKY WAY SATELLITE GALAXIES (2009, result): “We adopt a flat ΛCDM cosmology with matter density Ωm = 0.24, baryon density Ωb = 0.04, power spectrum normalization σ8 = 0.8, Hubble constant h = 0.7, and a primordial spectral index ns = 0.95, consistent with recent measurements (Spergel et al. 2007; Tegmark et al. 2006).”
THE COYOTE UNIVERSE. II. COSMOLOGICAL MODELS AND PRECISION EMULATION OF THE NONLINEAR MATTER POWER SPECTRUM (2009, background): “Recent determinations put the normalization in the range 0.7–0.9 with still rather large uncertainties (see, e.g., Vikhlinin et al. 2009 for constraints from clusters, Voevodkin & Vikhlinin 2004 for a low estimate from clusters, Tegmark et al. 2006 9 See http://lambda.gsfc.nasa.gov/.”
Environment and self-regulation in galaxy formation (2009, background): “This redshift range corresponds to a time interval of only 100 Myr at an average lookback time of 700 Myr adopting &m = 0.24, &' = 0.76 and H 0 = 73 km s−1 Mpc−1 (Tegmark et al. 2006; Percival et al. 2007) .”