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 nonlinear regime. The method, based on the dynamical evolution of the pair-conservation equation, relies on a universal relation between the pairwise 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.
|Original language||English (US)|
|Issue number||2 PART 2|
|State||Published - Feb 1 2001|
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
- Cosmology: theory