  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 ~3600 galaxies from the Calar Alto Deep Imaging Survey
(CADIS). The multicolor classification and redshift determination is reliable
up to I=23. The redshift distribution extends to z~1.1, the resolution is Delta
cz=12000 km s^-1. Thus the amplitude of the three-dimensional correlation
function has to 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). The LCRS also serves as ''local'' measurement. We
invented a new method to overcome the influence of redshift errors on w(r_p).
For evolution of the clustering strength the ansatz xi(r_com,z)proportional to
(1+z)^q is used. For the galaxies as a whole the evolution parameter turns out
to be q~-1.9, according to the prediction of linear theory. A formal dependency
on the cosmology is presumably due to the small number of fields observed.
However, the measured clustering growth clearly depends on Hubble type. At z~1
early type galaxies are already much stronger clustered, an increase with q~-1
is sufficient to explain the present day amplitude of the correlation function.
