  We present results of an investigation of clustering evolution of field
galaxies between a redshift of z\~1 and the present epoch. The current analysis
relies on a sample of ~14000 galaxies in two fields of the COMBO-17 survey. The
redshift distribution extends to z~1.1. The amplitude of the three-dimensional
correlation function can be estimated by means of the projected correlation
function w(r_p). The validity of the deprojection was tested on the Las
Campanas Redshift Survey (LCRS). In a flat cosmology with non-zero cosmological
constant for bright galaxies (M_B<-18) the clustering growth is proportional to
(1+z)^{-2}. However, the measured clustering evolution clearly depends on
Hubble type. While locally the clustering strength of early type galaxies is
equal to that of the bright galaxies, at high redshifts they are much stronger
clustered, and thus the clustering has to evolve much more slowly.
