Scaling in Gravitational Clustering, 2D and 3D Dynamics

Details Scaling in Gravitational Clustering, 2D and 3D Dynamics Scaling in Gravitational Clustering, 2D and 3D Dynamics

1997-07-01

arxiv.org/abs/astro-ph/9707009v1

Mon.Not.Roy.Astron.Soc. 303 (1999) 433-445

Astronomy and Astrophysics

Astrophysics

13 pages, Latex file, 9 Postscript Figures

Scientific paper

10.1046/j.1365-8711.1999.02167.x

Perturbation Theory (PT) applied to a cosmological density field with Gaussian initial fluctuations suggests a specific hierarchy for the correlation functions when the variance is small. In particular quantitative predictions have been made for the moments and the shape of the one-point probability distribution function (PDF) of the top-hat smoothed density. In this paper we perform a series of systematic checks of these predictions against N-body computations both in 2D and 3D with a wide range of featureless power spectra. In agreement with previous studies, we found that the reconstructed PDF-s work remarkably well down to very low probabilities, even when the variance approaches unity. Our results for 2D reproduce the features for the 3D dynamics. In particular we found that the PT predictions are more accurate for spectra with less power on small scales. The nonlinear regime has been explored with various tools, PDF-s, moments and Void Probability Function (VPF). These studies have been done with unprecedented dynamical range, especially for the 2D case, allowing in particular more robust determinations of the asymptotic behaviour of the VPF. We have also introduced a new method to determine the moments based on the factorial moments. Results using this method and taking into account the finite volume effects are presented.

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