EDP Sciences
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Volume 476, Number 1, December II 2007
Page(s) 31 - 58
Section Cosmology (including clusters of galaxies)
DOI http://dx.doi.org/10.1051/0004-6361:20078065

A&A 476, 31-58 (2007)
DOI: 10.1051/0004-6361:20078065

Using the Zeldovich dynamics to test expansion schemes

P. Valageas

Service de Physique Théorique, CEA Saclay, 91191 Gif-sur-Yvette, France
    e-mail: volag@spht.saclay.cea.fr

(Received 12 June 2007 / Accepted 24 August 2007)

Aims.We apply various expansion schemes that may be used to study gravitational clustering to the simple case of the Zeldovich dynamics.
Methods.Using the well-known exact solution of the Zeldovich dynamics we can compare the predictions of these various perturbative methods with the exact nonlinear result. We can also study their convergence properties and their behavior at high orders.
Results.We find that most systematic expansions fail to recover the decay of the response function in the highly nonlinear regime. "Linear methods" lead to increasingly fast growth in the nonlinear regime for higher orders, except for Padé approximants that give a bounded response at any order. "Nonlinear methods" manage to obtain some damping at one-loop order but they fail at higher orders. Although it recovers the exact Gaussian damping, a resummation in the high-k limit is not justified very well as the generation of nonlinear power does not originate from a finite range of wavenumbers (hence there is no simple separation of scales). No method is able to recover the relaxation of the matter power spectrum on highly nonlinear scales. It is possible to impose a Gaussian cutoff in a somewhat ad-hoc fashion to reproduce the behavior of the exact two-point functions for two different times. However, this cutoff is not directly related to the clustering of matter and disappears in exact equal-time statistics such as the matter power spectrum. On a quantitative level, on weakly nonlinear scales, the usual perturbation theory, and the nonlinear scheme to which one adds an ansatz for the response function with such a Gaussian cutoff, are the two most efficient methods. We can expect these results to hold for the gravitational dynamics as well (this has been explicitly checked at one-loop order), since the structure of the equations of motion is identical for both dynamics.

Key words: gravitation -- cosmology: theory -- large-scale structure of Universe

© ESO 2007