Non-Gaussianity of the density distribution in accelerating universes

Details Non-Gaussianity of the density distribution in accelerating universes Non-Gaussianity of the density distribution in accelerating universes

2005-11-24

arxiv.org/abs/astro-ph/0511688v2

JCAP 0602:006,2006

Astronomy and Astrophysics

Astrophysics

15 pages, 4 figures, accepted for publication in JCAP; v2: smoothing scale has been changed

Scientific paper

10.1088/1475-7516/2006/02/006

According to recent observations, the existence of the dark energy has been considered. Even though we have obtained the constraint of the equation of the state for dark energy ($p = w \rho$) as $-1 \le w \le -0.78$ by combining WMAP data with other astronomical data, in order to pin down $w$, it is necessary to use other independent observational tools. For this purpose, we consider the $w$ dependence of the non-Gaussianity of the density distribution generated by nonlinear dynamics. To extract the non-Gaussianity, we follow a semi-analytic approach based on Lagrangian linear perturbation theory, which provides an accurate value for the quasi-nonlinear region. From our results, the difference of the non-Gaussianity between $w = -1$ and $w= -0.5$ is about 4% while that between $w = -1$ and $w= -0.8$ is about $0.9 %$. For the highly non-linear region, we estimate the difference by combining this perturbative approach with N-body simulation executed for our previous paper. From this, we can expect the difference to be more enhanced in the low-$z$ region, which suggests that the non-Gaussianity of the density distribution potentially plays an important role for extracting the information of dark energy.

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