Simulation of Large-Scale Structure of Universe by Gaussian Random
  Fields
  Large-scale structure of Universe includes galaxy clusters connected by
filaments. Voids occupy the rest of cosmic volume. The search of any
dependencities in filament structure can give answer to more general questions
about origin of structures in the Universe. This becomes possible because,
according to current picture of Universe, one could simulate the evolution of
Universe until its very beginning or vice versa. According to current
cosmological hydrodynamical theories a number of computer simulations of LSS
were performed to describe its properties. In this work we consider alternative
variant of simulating the distribution of matter that is very similar to real.
We simulated two-dimensional galaxy distribution on the sky using random
distributions of clusters and single galaxies. The main assumption was that
matter clusterised to initial density fluctuations with uniform distribution.
According to Zeldovich theory, low-dimensional anisotropies should increase,
that corresponds to appearance of filaments in 2D case. Thus we generated a net
of filaments between clusters with certain length limits. Real galaxy
distribution was simulated by random changing galaxy positions in filaments and
clusters. We generated radial distributions of galaxies in clusters taking into
account the surrounding and add uniform distribution of isolated galaxies in
voids. Our model has been coordinated with SDSS galaxy distribution with using
two-point angular correlation function. Parameters of random distributions were
found for the case of equality of correlation function slope for the model and
for observational data.
