A Simple Method for Computing the Non-Linear Mass Correlation Function with Implications for Stable Clustering

Abstract

We propose a simple and accurate method for computing analytically the mass correlation function for cold dark matter and scale-free models that fits N-body simulations over a range that extends from the linear to the strongly non-linear regime. The method, based on the dynamical evolution of the pair conservation equation, relies on a universal relation between the pair-wise velocity and the smoothed correlation function valid for high and low density models, as derived empirically from N-body simulations. An intriguing alternative relation, based on the stable-clustering hypothesis, predicts a power-law behavior of the mass correlation function that disagrees with N-body simulations but conforms well to the observed galaxy correlation function if negligible bias is assumed. The method is a useful tool for rapidly exploring a wide span of models and, at the same time, raises new questions about large scale structure formation.

10 pages, 3 figures

References in corpus (2)

• The Mass Power Spectrum in Quintessence Cosmological Models
• The Dependence of Velocity and Clustering Statistics on Galaxy Properties

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