astro-ph 9403028 PROPERTIES OF THE COSMOLOGICAL DENSITY DISTRIBUTION FUNCTION by

The properties of the probability distribution function of the cosmological continuous density eld are studied. We present further developments and compare dynamically motivated methods to derive the PDF. One of them is based on the Zel'dovich approximation (ZA). We extend this method for arbitrary initial conditions, regardless of whether they are Gaussian or not. The other approach is based on perturbation theory with Gaussian initial uctuations. We include the smoothing e ects in the PDFs. We examine the relationships between the shapes of the PDFs and the moments. It is found that formally there are no moments in the ZA, but a way to resolve this issue is proposed, based on the regularization of integrals. A closed form for the generating function of the moments in the ZA is also presented, including the smoothing e ects. We suggest the methods to build PDFs out of the whole series of the moments, or out of a limited number of moments { the Edgeworth expansion. The last approach gives us an alternative method to evaluate the skewness and kurtosis by measuring the PDF around its peak. We note a general connection between the generating function of moments for small r.m.s and the non-linear evolution of the overdense spherical uctuation in the dynamical models. All these approaches have been applied in 1D case where the ZA is exact, and simple analytical results are obtained. It allows us to study in details how these methods are related to each other. The 3D case is analyzed in the same manner and we found a mutual agreement in the PDFs derived by di erent methods in the the quasi-linear regime. Numerical CDM simulation was used to validate the accuracy of considered approximations. We explain the successful log-normal t of the PDF from that simulation at moderate as mere fortune, but not as a universal form of density PDF in general. Subject headings: cosmology: theory | dark matter | galaxies: clustering