Biasing phenomenon
  We study biasing as a physical phenomenon by analysing power spectra (PS) and
correlation functions (CF) of simulated galaxy samples and dark matter (DM)
samples. We apply an algorithm based on the local densities of particles,
$\rho$, to form populations of simulated galaxies, using particles with $\rho
\ge \rho_0$. We calculate two-point CF of projected (2D) and spatial (3D)
density fields of simulated galaxies for various particle-density limits
$\rho_0$. We compare 3D and 2D CFs; in 2D case we use samples of various
thickness to find the dependence of 2D CFs on thickness of samples. Dominant
elements of the cosmic web are clusters and filaments, separated by voids
filling most of the volume. In individual 2D sheets positions of clusters and
filaments do not coincide. As a result, in projection clusters and filaments
fill in 2D voids. This leads to the decrease of amplitudes of CFs in
projection. For this reason amplitudes of 2D CFs are lower than amplitudes of
3D CFs, the difference is the larger, the thicker are 2D samples. Using PS and
CFs of simulated galaxies and DM we estimate the bias factor for $L^\ast$
galaxies, $b^\ast =1.85 \pm 0.15$.
