Experimental Cosmic Statistics II: Distribution

Abstract

Colombi et al. 1999 (paper I) investigated the counts-in-cells statistics and their respective errors in the $τ$CDM Virgo Hubble Volume simulation. This extremely large $N$-body experiment also allows a numerical investigation of the {\em cosmic distribution function}, $Υ(\tA)$ itself for the first time. For a statistic $A$, $Υ(\tA)$ is the probability density of measuring the value $\tA$ in a finite galaxy catalog. $Υ$ was evaluated for the distribution of counts-in-cells, $P_N$, the factorial moments, $F_k$, and the cumulants, $\xiav$ and $S_N$'s, using the same subsamples as paper I. While paper I concentrated on the first two moments of $Υ$, i.e. the mean, the cosmic error and the cross-correlations, here the function $Υ$ is studied in its full generality, including a preliminary analysis of joint distributions $Υ(\tA,\tB)$. The most significant, and reassuring result for the analyses of future galaxy data is that the cosmic distribution function is nearly Gaussian provided its variance is small. A good practical criterion for the relative cosmic error is that $ΔA/A \la 0.2$. This means that for accurate measurements, the theory of the cosmic errors, presented by Szapudi & Colombi (1996) and Szapudi, Colombi & Bernardeau (1999), and confirmed empirically by paper I, is sufficient for a full statistical description and thus for a maximum likelihood rating of models. As the cosmic error increases, the cosmic distribution function $Υ$ becomes increasingly skewed and is well described by a generalization of the lognormal distribution. The cosmic skewness is introduced as an additional free parameter. (...more in paper...)