Experimental Cosmic Statistics II: Distribution

Details Experimental Cosmic Statistics II: Distribution Experimental Cosmic Statistics II: Distribution

1999-12-10

arxiv.org/abs/astro-ph/9912238v1

Astronomy and Astrophysics

Astrophysics

Latex, 11 pages, 8 postscript figures. Accepted for pulication in MNRAS

Scientific paper

10.1046/j.1365-8711.2000.03256.x

Colombi et al. 1999 (paper I) investigated the counts-in-cells statistics and their respective errors in the $\tau$CDM Virgo Hubble Volume simulation. This extremely large $N$-body experiment also allows a numerical investigation of the {\em cosmic distribution function}, $\Upsilon(\tA)$ itself for the first time. For a statistic $A$, $\Upsilon(\tA)$ is the probability density of measuring the value $\tA$ in a finite galaxy catalog. $\Upsilon$ 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 $\Upsilon$, i.e. the mean, the cosmic error and the cross-correlations, here the function $\Upsilon$ is studied in its full generality, including a preliminary analysis of joint distributions $\Upsilon(\tA,\tB)$. 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 $\Delta A/A \la 0.2$. 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 $\Upsilon$ 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...)

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