We present results from an investigation of the clustering evolution of field galaxies between a redshift of z \sim 1 and the present epoch .
The current analysis relies on a sample of \sim 3600 
galaxies from the C alar A lto D eep I maging S urvey ( CADIS ) .
Its multicolor classification and redshift determination is reliable up to I = 23 ^ { mag } .
The redshift distribution extends to z \sim 1.1 , with formal errors of \sigma _ { z } \simeq 0.02 .
Thus 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 ) , which also serves as a “ local ” measurement .
We developed a new method to overcome the influence of redshift errors on w ( r _ { p } ) .
We parametrise the evolution of the clustering strength with redshift by a parameter q , the values of which give directly the deviation of the evolution from the global Hubble flow : \xi ( r _ { \mathrm { comoving } } = 1 h ^ { -1 } \mathrm { Mpc } ) = \xi _ { 0 } ( 1 + z ) ^ { q } .
From a subsample of bright galaxies we find q = -3.44 \pm 0.29 ( for \Omega _ { m } = 1 , \Omega _ { \Lambda } = 0 ) , -2.84 \pm 0.30 ( for \Omega _ { m } = 0.2 , \Omega _ { \Lambda } = 0 ) , and q = -2.28 \pm 0.31 ( for \Omega _ { m } = 0.3 , \Omega _ { \Lambda } = 0.7 ) , that is a significant growth of the clustering strength between z = 1 and the present epoch .
From linear theory of dark matter clustering growth one would only expect q = -2 
for a flat high-density model .
Moreover , we establish that the measured clustering strength depends on galaxy type : galaxies with early type SED s ( Hubble type : E0 to Sbc ) are more strongly clustered at redshifts z \ga 0.2 than later types .
The evolution of the amplitude of the two-point correlation function for these “ old ” galaxies is much slower ( q = -0.85 \pm 0.82 for \Omega _ { m } = 0.3 , \Omega _ { \Lambda } = 0.7 ) .
Since the evolution of the clustering of bright and early type galaxies seems to converge to the same value in the local universe , we conclude that the apparent strong evolution of clustering among all bright galaxies is dominated by the effect that weakly clustered starburst galaxies which are common at high redshifts z \approx 1.0 have dimmed considerably since then .
Thus the true clustering of massive galaxies is better followed by the early types .
This provides both a natural explanation for the seemingly conflicting results of previous studies and accords with the absence of ” faint blue galaxies ” in the local universe .