Non-gaussian Features of Linear Cosmic String Models

Details Non-gaussian Features of Linear Cosmic String Models Non-gaussian Features of Linear Cosmic String Models

1998-03-11

arxiv.org/abs/astro-ph/9803120v2

Astrophys.J.507:L101-L104,1998

Astronomy and Astrophysics

Astrophysics

6 pages, 6 figures; accepted by Ap. J. Lett. With error bars included in the genus curves (figure 3). Also corrected for a min

Scientific paper

10.1086/311686

We investigate the non-gaussian properties of cosmic-string-seeded linear density perturbations with cold and hot dark matter backgrounds, using high-resolution numerical simulations. We compute the one-point probability density function of the resulting density field, its skewness, kurtosis, and genus curves for different smoothing scales. A semi-analytic model is then invoked to provide a physical interpretation of our results. We conclude that on scales smaller than $1.5{(\Omega h^2)}^{-1}$Mpc, perturbations seeded by cosmic strings are very non-gaussian. These scales may still be in a linear or mildly non-linear regime in an open or $\Lambda$-universe with $\Gamma=\Omega h \lsim 0.2$.

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