How well can (renormalized) perturbation theory predict dark matter clustering properties?

Abstract

There has been some recent activity in trying to understand the dark matter clustering properties in the quasilinear regime, through resummation of perturbative terms, otherwise known as the renormalized perturbation theory (astro-ph/0509418), or the renormalization group method (astro-ph/0606028). While it is not always clear why such methods should work so well, there is no reason for them to capture non-perturbative events such as shell-crossing. In order to estimate the magnitude of non-perturbative effects, we introduce a (hypothetical) model of sticky dark matter, which only differs from collisionless dark matter in the shell-crossing regime. This enables us to show that the level of non-perturbative effects in the dark matter power spectrum at k ~ 0.1 Mpc^{-1}, which is relevant for baryonic acoustic oscillations, is about a percent, but rises to order unity at k ~ 1 Mpc^{-1}.

3 pages, 3 figures, submitted to PRD (rapid communication)

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Cited by in corpus (18)

• Nonlinear Evolution of Baryon Acoustic Oscillations
• A critical look at cosmological perturbation theory techniques
• Generation of Vorticity and Velocity Dispersion by Orbit Crossing
• Resumming Cosmic Perturbations
• A Closure Theory for Non-linear Evolution of Cosmological Power Spectra
• Dark matter clustering: a simple renormalization group approach
• Coarse-Grained Cosmological Perturbation Theory
• Cosmological perturbation theory in 1+1 dimensions
• The Mildly Non-Linear Regime of Structure Formation
• Baryonic Acoustic Oscillations via the Renormalization Group
• Impact of shell crossing and scope of perturbative approaches in real and redshift space
• Renormalized Newtonian Cosmic Evolution with Primordial Non-Gaussianity
• Large-scale structure perturbation theory without losing stream crossing
• Universality of shear-banding instability and crystallization in sheared granular fluid
• Divergence of Perturbation Theory in Large Scale Structures
• Accuracy of analytical models of the large-scale matter distribution
• The Helmholtz Hierarchy: Phase Space Statistics of Cold Dark Matter
• Kinetic Field Theory: Perturbation theory beyond first order