Simulations of Baryon Acoustic Oscillations II: Covariance matrix of the matter power spectrum

Abstract

We use 5000 cosmological N-body simulations of 1(Gpc/h)^3 box for the concordance LCDM model in order to study the sampling variances of nonlinear matter power spectrum. We show that the non-Gaussian errors can be important even on large length scales relevant for baryon acoustic oscillations (BAO). Our findings are (1) the non-Gaussian errors degrade the cumulative signal-to-noise ratios (S/N) for the power spectrum amplitude by up to a factor of 2 and 4 for redshifts z=1 and 0, respectively. (2) There is little information on the power spectrum amplitudes in the quasi-nonlinear regime, confirming the previous results. (3) The distribution of power spectrum estimators at BAO scales, among the realizations, is well approximated by a Gaussian distribution with variance that is given by the diagonal covariance component. (4) For the redshift-space power spectrum, the degradation in S/N by non-Gaussian errors is mitigated due to nonlinear redshift distortions. (5) For an actual galaxy survey, the additional shot noise contamination compromises the cosmological information inherent in the galaxy power spectrum, but also mitigates the impact of non-Gaussian errors. The S/N is degraded by up to 30% for a WFMOS-type survey. (6) The finite survey volume causes additional non-Gaussian errors via the correlations of long-wavelength fluctuations with the fluctuations we want to measure, further degrading the S/N values by about 30% even at high redshift z=3.

submitted to ApJ, 14 pages, 12 figures. The full halo model is included. Minor changes also made, and references added

References in corpus (22)

• Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology
• Measuring the Baryon Acoustic Oscillation scale using the SDSS and 2dFGRS
• Resumming Cosmological Perturbations via the Lagrangian Picture: One-loop Results in Real Space and in Redshift Space
• Nonlinear Evolution of Baryon Acoustic Oscillations
• Cosmology and the Bispectrum
• The Scale Dependence of Halo and Galaxy Bias: Effects in Real Space
• Flowing with Time: a New Approach to Nonlinear Cosmological Perturbations
• Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies
• The detectability of baryonic acoustic oscillations in future galaxy surveys
• A Closure Theory for Non-linear Evolution of Cosmological Power Spectra
• Non-linear structure formation and the acoustic scale
• Dark matter clustering: a simple renormalization group approach
• Cosmic Calibration: Constraints from the Matter Power Spectrum and the Cosmic Microwave Background
• Perturbation Theory Reloaded II: Non-linear Bias, Baryon Acoustic Oscillations and Millennium Simulation In Real Space
• Simulations of Baryon Oscillations
• Third-Order Density Perturbation and One-Loop Power Spectrum in Dark-Energy-Dominated Universe
• Baryonic Acoustic Oscillations via the Renormalization Group
• Information content in the halo-model dark-matter power spectrum
• Systematic effects in the sound horizon scale measurements
• Simulations of Baryon Acoustic Oscillations I: Growth of Large-Scale Density Fluctuations
• Information Content in the Galaxy Angular Power Spectrum from the Sloan Digital Sky Survey and Its Implication on Weak Lensing Analysis
• Baryon oscillations in galaxy and matter power-spectrum covariance matrices

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