Non-Gaussian features of linear cosmic string models

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 and its skewness, kurtosis, and genus curves for different smoothing scales. A semianalytic model is then invoked to provide a physical interpretation of our results. We conclude that on scales smaller than 1.5(Ohm h(2))(-1) Mpc, perturbations seeded by cosmic strings are very non-Gaussian. These scales may still be in a linear or mildly nonlinear regime in an open or Lambda universe with Gamma = Ohm h less than or similar to 0.2.