  Recent development of galaxy surveys enables us to investigate the deep
universe of high redshift. We quantitatively present the physical information
extractable from the observable correlation function in deep redshift space in
a framework of the linear theory. The correlation function depends on the
underlying power spectrum, velocity distortions, and the Alcock-Paczy\'nski
(AP) effect. The underlying power spectrum is sensitive to the constituents of
matters in the universe, the velocity distortions are sensitive to the galaxy
bias as well as the amount of total matter, and the Alcock-Paczy\'nski effect
is sensitive to the dark energy components. Measuring the dark energy by means
of the baryonic feature in the correlation function is one of the most
interesting applications. We show that the ``baryon ridge'' in the correlation
function serves as a statistically circular object in the AP effect. In order
to sufficiently constrain the dark energy components, the redshift range of the
galaxy survey should be as broad as possible. The survey area on the sky should
be smaller at deep redshifts than at shallow redshifts to keep the number
density as dense as possible. We illustrate an optimal survey design that are
useful in cosmology. Assuming future redshift surveys of $z\simlt 3$ which are
within reach of the present-day technology, achievable error bounds on
cosmological parameters are estimated by calculating the Fisher matrix.
According to an illustrated design, the equation of state of dark energy can be
constrained within $\pm 5%$ error assuming that the bias is unknown and
marginalized over. Even when all the other cosmological parameters should be
simultaneously determined, the error bound for the equation of state is up to
$\pm 10%$.
