Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies (vol 404, pg 60, 2010)

By B. Reid, Will J. Percival, Daniel J. Eisenstein, L. Verde, David N. Spergel, R. Skibba, N. Bahcall, Tamás Budavári, M. Fukugita, J. Richard Gott III and 18 more. 2009

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We present the power spectrum of the reconstructed halo density field derived from a sample of luminous red galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) Seventh Data Release (DR7). The halo power spectrum has a direct connection to the underlying dark matter power for k≤ 0.2 h Mpc−1, well into the quasi-linear regime. This enables us to use a factor of ∼8 more modes in the cosmological analysis than an analysis with kmax= 0.1 h Mpc−1, as was adopted in the SDSS team analysis of the DR4 LRG sample. The observed halo power spectrum for 0.02 < k < 0.2 h Mpc−1 is well fitted by our model: χ2= 39.6 for 40 degrees of freedom for the best-fitting Λ cold dark matter (ΛCDM) model. We find Ωmh2(ns/0.96)1.2= 0.141+0.101-0.012 for a power-law primordial power spectrum with spectral index ns and Ωbh2= 0.022 65 fixed, consistent with cosmic microwave background measurements. The halo power spectrum also constrains the ratio of the comoving sound horizon at the baryon-drag epoch to an effective distance to z= 0.35: rs/DV(0.35) = 0.1097+0.0039−0.0042. Combining the halo power spectrum measurement with the Wilkinson Microwave Anisotropy Probe (WMAP) 5 year results, for the flat ΛCDM model we find Ωm= 0.289 ± 0.019 and H0= 69.4 ± 1.6 km s−1 Mpc−1. Allowing for massive neutrinos in ΛCDM, we find Σmv <0.62 eV at the 95 per cent confidence level. If we instead consider the effective number of relativistic species Neff as a free parameter, we find Neff= 4.8+1.8−1.7. Combining also with the Kowalski et al. supernova sample, we find Ωtot= 1.011 ± 0.009 and w=−0.99 ± 0.11 for an open cosmology with constant dark energy equation of state w. The power spectrum and a module to calculate the likelihoods are publicly available at http://lambda.gsfc.nasa.gov/toolbox/lrgdr/.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a10800372929f3fe7de462c8150854c736d24c43

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Citations in the corpus

The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity (2012, methodology): “We measure the power spectrum, Pm(k), using the standard Fourier technique of Feldman et al. (1994), as described in Reid et al. (2010) and Anderson et al. (2012).”
THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM (2010, methodology): “Recent constraints on the number of relativistic species have been explored with CMB data from WMAP combined with low redshift probes by e.g., Spergel et al. (2007); Ichikawa et al. (2007); Mangano et al. (2007); Hamann et al. (2007); Dunkley et al. (2009); Komatsu et al. (2010); Reid et al. (2010).”
Modelling the anisotropic two-point galaxy correlation function on small scales and single-probe measurements of H(z), DA(z) and f(z)σ8(z) from the Sloan Digital Sky Survey DR7 luminous red galaxies (2012, methodology): “…both the powerspectrum method (see e.g. Tegmark et al. 2004; Hutsi 2005; Blake et al. 2007; Padmanabhan et al. 2007; Percival et al. 2007, 2010; Reid et al. 2010; Montesano, Sanchez & Phleps 2012) and the correlation function method (see e.g. Eisenstein et al. 2005; Okumura et al. 2008; Cabre…”
The 6dF Galaxy Survey: baryon acoustic oscillations and the local Hubble constant (2011, methodology): “…Hui 2009; Labini et al. 2009; Sanchez et al. 2009; Kazin et al. 2010), the power spectrum P (k) (Cole et al. 2005; Tegmark et al. 2006; Huetsi 2006; Reid et al. 2010), the projected correlation function w(rp) of photometric redshift samples (Padmanabhan et al. 2007; Blake et al. 2007) and a…”
SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, methodology): “Note that the DR7 constraint has almost no effect on the uncertainty in the measurement of w – WMAP7+H0+SNLS3 has essentially the same uncertainty as WMAP7+DR7+H0+SNLS3.”
The clustering of galaxies in the SDSS‐III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large‐scale two‐point correlation function (2012, background): “…of the Universe or details of inflationary physics (Percival et al. 2002; Tegmark et al. 2004; Cole et al. 2005; Sánchez et al. 2006; Spergel et al. 2007; Komatsu et al. 2009; Komatsu 2010; Percival et al. 2010; Reid et al. 2010a; Keisler et al. 2011; Blake et al. 2011; Montesano et al. 2012).”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, unknown): “Cosmological models based on CDM reproduce the spatial clustering of galaxies on large scales quite well (Reid et al. 2010) and even the clustering of galaxies on∼ 1 Mpc scales appears to match that expected for CDMsubhalos (Kravtsov et al. 2004; Conroy et al. 2006; Trujillo-Gomez et al. 2011;…”
MontePython 3: Boosted MCMC sampler and other features (2018, background): “0 SC [81] [54] simlow from Planck 2016: TTTEEE low ` τreio prior 3.”
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, background): “The shape of the measured correlation function (Reid et al. 2010) or the power-spectrum (Montesano, Sanchez & Phleps 2011), analogously to the shape of the measured CMB power-spectrum (Larson et al. 2011), can be used to constrain basic cosmological parameters.”
Self-Interacting Dark Matter from a Non-Abelian Hidden Sector (2014, methodology): “[28] B.”
Galaxy UV-luminosity function and reionization constraints on axion dark matter (2014, background): “Cosmological probes of the linear regime of structure formation, such as the power spectrum, P (k), of density fluctuations (e.g. Reid et al. 2010) and the Cosmic Microwave Background (CMB, e.g. Ade et al. 2013a), provide only weak constraints on the mass of the DM particle (warm or axion-like) in…”
Local gravity versus local velocity: solutions for β and non-linear bias (2010, unknown): “Taking σ 8g = 0.97 ± 0.05 (Westover 2007; Reid et al. 2010) yields σ 8 = σ 8g/b = 0.65 ± 0.11 for the underlying mass density field, marginally consistent with the latest Wilkinson Microwave Anisotropy Probe (WMAP) results (Larson et al. 2011) of σ 8 = 0.8 ± 0.03 (see also Jarosik et al. (2010)).”
The clustering of the SDSS DR7 Main Galaxy Sample I: a 4 per cent distance measure at z=0.15 (2014, methodology): “…and then summed into 8 h−1Mpc bins, allowing different choices for bin centres . c© 2014 RAS, MNRAS 000, 1–13 We measure the spherically-averaged power spectrum, P (k), using the standard Fourier technique of Feldman et al. (1994), as described in Reid et al. (2010) and Anderson et al. (2012).”