We measured the two dimensional galaxy–galaxy correlation function from the Muenster Red Sky Survey ( Ungruhe 1999 ) .
This survey has a slightly larger surface as the APM survey and complete up to r _ { F } < 18.3 mag ( z _ { med } \sim 0.14 ) .
The large dynamical range of the survey made it possible to examine sub-catalogues with different limiting magnitudes .
The positive part of our measured angular correlation functions ( after the colour correction ) agree excellently with those measured by Maddox , Efstathiou and Shutherland 1996 from the APM galaxy catalogue ( Maddox et al .
1990 ) .
From the measured angular correlation functions the three dimensional two-point correlation function \xi ( r ) was calculated .
We have chosen the evolution parameter \epsilon so that the change of the correlation length r _ { 0 } with the depth of the sub-catalogue were minimal .
This prescription gives r _ { 0 } = 5.82 \pm 0.05 h ^ { -1 } Mpc and a very high , positive evolution parameter \epsilon = 2.6 .
The position of the point , where the 3d correlation function breaks away from the power law depends on the depth of the sub-catalogues : for low magnitude limits the break-down comes earlier , for higher later .