Simulations of Baryon Acoustic Oscillations I: Growth of Large-Scale Density Fluctuations

Abstract

We critically examine how well the evolution of large-scale density perturbations is followed in cosmological $N$-body simulations. We first run a large volume simulation and perform a mode-by-mode analysis in three-dimensional Fourier space. We show that the growth of large-scale fluctuations significantly deviates from linear theory predictions. The deviations are caused by {\it nonlinear} coupling with a small number of modes at largest scales owing to finiteness of the simulation volume. We then develop an analytic model based on second-order perturbation theory to quantify the effect. Our model accurately reproduces the simulation results. For a single realization, the second-order effect appears typically as ``zig-zag'' patterns around the linear-theory prediction, which imprints artificial ``oscillations'' that lie on the real baryon-acoustic oscillations. Although an ensemble average of a number of realizations approaches the linear theory prediction, the dispersions of the realizations remain large even for a large simulation volume of several hundred megaparsecs on a side. For the standard $\Lambda$CDM model, the deviations from linear growth rate are as large as 10 percent for a simulation volume with $L=500h^{-1}$Mpc and for a bin width in wavenumber of $\Delta k=0.005h$Mpc${}^{-1}$, which are comparable to the intrinsic variance of Gaussian random realizations. We find that the dispersions scales as $\propto L^{-3/2}\Delta k^{-1/2}$ and that the mean dispersion amplitude can be made smaller than a percent only if we use a very large volume of $L>2h^{-1}$Gpc. The finite box size effect needs to be appropriately taken into account when interpreting results from large-scale structure simulations for future dark energy surveys using baryon acoustic oscillations.

arXiv commentreferences added, minor changes

References in corpus (35)

• Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology
• The cosmological simulation code GADGET-2
• Simulating the joint evolution of quasars, galaxies and their large-scale distribution
• Efficient Computation of CMB anisotropies in closed FRW models
• Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies
• The 2dF Galaxy Redshift Survey: Power-spectrum analysis of the final dataset and cosmological implications
• Large-Scale Structure of the Universe and Cosmological Perturbation Theory
• GADGET: A code for collisionless and gasdynamical cosmological simulations
• Power Spectra for Cold Dark Matter and its Variants
• Measuring the Baryon Acoustic Oscillation scale using the SDSS and 2dFGRS
• Probing Dark Energy with Baryonic Acoustic Oscillations from Future Large Galaxy Redshift Surveys
• Transients from Initial Conditions in Cosmological Simulations
• Resumming Cosmological Perturbations via the Lagrangian Picture: One-loop Results in Real Space and in Redshift Space
• Nonlinear Evolution of Baryon Acoustic Oscillations
• Cosmic Complementarity: H_0 and Omega_m from Combining CMB Experiments and Redshift Surveys
• Second Order Power Spectrum and Nonlinear Evolution at High Redshift
• The Scale Dependence of Halo and Galaxy Bias: Effects in Real Space
• Power Spectrum Correlations Induced by Non-Linear Clustering
• Baryonic acoustic oscillations in simulated galaxy redshift surveys
• Large-Scale Anisotropic Correlation Function of SDSS Luminous Red Galaxies
• Perturbation Theory Reloaded: Analytical Calculation of Non-linearity in Baryonic Oscillations in the Real Space Matter Power Spectrum
• The detectability of baryonic acoustic oscillations in future galaxy surveys
• Multi-Point Propagators in Cosmological Gravitational Instability
• A Closure Theory for Non-linear Evolution of Cosmological Power Spectra
• Correlation Function in Deep Redshift Space as a Cosmological Probe
• The Growth of Correlations in the Matter Power Spectrum
• Dark matter clustering: a simple renormalization group approach
• Self-Similar Evolution of Cosmological Density Fluctuations
• Bispectrum and Nonlinear Biasing of Galaxies: Perturbation Analysis, Numerical Simulation and SDSS Galaxy Clustering
• Simulations of Baryon Oscillations
• Self-Similar Evolution of Gravitational Clustering: N-Body Simulations of the n=-2 Spectrum
• Systematic effects in the sound horizon scale measurements
• Effects of the size of cosmological N-Body simulations on physical quantities -- I: Mass Function
• Statistics of Fourier Modes in Non-Gaussian Fields
• Baryon oscillations in galaxy and matter power-spectrum covariance matrices

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