  The observed two-point correlation functions of galaxies in redshift space
become anisotropic due to the geometry of the universe as well as due to the
presence of the peculiar velocity field. On the basis of linear perturbation
theory, we expand the induced anisotropies of the correlation functions with
respect to the redshift $z$, and obtain analytic formulae to infer the
deceleration parameter $q_0$, the density parameter $\Omega_0$ and the
derivative of the bias parameter $d\ln b/dz$ at $z=0$ in terms of the
observable statistical quantities. The present method does not require any
assumption of the shape and amplitude of the underlying fluctuation spectrum,
and thus can be applied to future redshift surveys of galaxies including the
Sloan Digital Sky Survey. We also evaluate quantitatively the systematic error
in estimating the value of $\beta_0 \equiv \Omega_0^{0.6}/b$ from a galaxy
redshift survey on the basis of a conventional estimator for $\beta_0$ which
neglects both the geometrical distortion effect and the time evolution of the
parameter $\beta(z)$. If the magnitude limit of the survey is as faint as 18.5
(in B-band) as in the case of the Sloan Digital Sky Survey, the systematic
error ranges between -20% and 10% depending on the cosmological parameters.
Although such systematic errors are smaller than the statistical errors in the
current surveys, they will dominate the expected statistical error for future
surveys.
