Cosmological Parameters from Eigenmode Analysis of Sloan Digital Sky Survey Galaxy Redshifts

By Adrian Pope, Takahiko Matsubara, A. Szalay, M. Blanton, Daniel J. Eisenstein, Jim Gray, B. Jain, N. Bahcall, J. Brinkmann, Tamás Budavári and 16 more. 2004

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We present estimates of cosmological parameters from the application of the Karhunen-Loève transform to the analysis of the three-dimensional power spectrum of density fluctuations using Sloan Digital Sky Survey galaxy redshifts. We use Ωmh and fb = Ωb/Ωm to describe the shape of the power spectrum, σ for the (linearly extrapolated) normalization, and β to parameterize linear theory redshift-space distortions. On scales k ≲ 0.16 h Mpc-1, our maximum likelihood values are Ωmh = 0.264 ± 0.043, fb = 0.286 ± 0.065, σ = 0.966 ± 0.048, and β = 0.45 ± 0.12. When we take a prior on Ωb from the Wilkinson Microwave Anisotropy Probe (WMAP), we find Ωmh = 0.207 ± 0.030, which is in excellent agreement with WMAP and the Two-Degree Field. This indicates that we have reasonably measured the gross shape of the power spectrum, but we have difficulty breaking the degeneracy between Ωmh and fb, because the baryon oscillations are not resolved in the current spectroscopic survey window function.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e69a31005c9a066f5c10d15cb71a920467874303

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Citations in the corpus

REJUVENATING THE MATTER POWER SPECTRUM: RESTORING INFORMATION WITH A LOGARITHMIC DENSITY MAPPING (2009, unknown): “0.2hMpc−1 (e.g., Pope et al. 2004; Tegmark et al. 2006).”
New York University Value-Added Galaxy Catalog: A Galaxy Catalog Based on New Public Surveys (2004, background): “…the luminosity function, power spectrum, correlation function, and a number of other galaxy property and galaxy clustering statistics (e.g., Blanton et al. 2003c; Tegmark et al. 2004; Zehavi et al. 2002; Hogg et al. 2003; Hoyle et al. 2005; Shen et al. 2003; Baldry et al. 2004; Pope et al. 2004).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “…size of these maps of the galaxy distribution has permitted the most accurate measurements to date of the power spectrum of galaxy clustering (Percival et al. 2001; Tegmark et al. 2004a; Pope et al. 2004; Cole et al. 2005; Padmanabhan et al. 2006; Percival et al. 2006a; Tegmark et al. 2006).”
Cosmological baryonic and matter densities from 600 000 SDSS luminous red galaxies with photometric redshifts (2006, background): “Measurements of large-scale structure have continued to constitute an important component of cosmological parameter fits (e.g. Efstathiou et al. 2002; Percival et al. 2002; Spergel et al. 2003; Pope et al. 2004; Tegmark et al. 2004b; Seljak et al. 2005; Sanchez et al. 2006).”
The Shape of the Sloan Digital Sky Survey Data Release 5 Galaxy Power Spectrum (2007, methodology): “Similar values of M ’ 0:3 were found by alternative analyses of the red-selected SDSS main galaxy power spectrum (Pope et al. 2004), a set of SDSS spectroscopic LRGs (Eisenstein et al. 2005), and SDSSphotometrically selected LRGs (Padmanabhan et al. 2006; Blake et al. 2007).”
Cosmological parameters from supernova observations: A critical comparison of three data sets (2003, background): “…this in mind, we fix the value ofΩm to 0.2, 0.3 and 0.4 (which are typical range of values determined by other observations, like the LSS surveys, and are independent of thenature of the dark energy; Pope et al. 2004; Tegmark et al. 2004b; Tegmark et al. 2004a), and marginalize only overM1,2.”
Cosmological parameters from cosmic microwave background measurements and the final 2dF Galaxy Redshift Survey power spectrum (2006, background): “Other papers have also analysed the information encoded in the 2dFGRS and SDSS power spectra (Tegmark, Zaldarriaga & Hamilton 2001; Pope et al. 2004; Tegmark et al. 2004b; Seljak et al. 2005).”