We present B , R , and I -band selected galaxy catalogues based on the Munich Near-Infrared Cluster Survey ( MUNICS ) which , together with the previously used K -selected sample , serve as an important probe of galaxy evolution in the redshift range 0 \la z \la 2 .
Furthermore , used in comparison they are ideally suited to study selection effects in extragalactic astronomy .
The construction of the B , R , and I -selected photometric catalogues , containing \sim 9000 , \sim 9000 , and \sim 6000 galaxies , respectively , is described in detail .
The catalogues reach 50 % completeness limits for point sources of B \simeq 24.5 mag , R \simeq 23.5 mag , and I \simeq 22.5 mag and cover an area of about 0.3 square degrees .
Photometric redshifts are derived for all galaxies with an accuracy of \delta z / ( 1 + z ) \simeq 0.057 , very similar to the K -selected sample .
Galaxy number counts in the B , V , R , I , J , and K bands demonstrate the quality of the dataset .

The rest-frame colour distributions of galaxies at different selection bands and redshifts suggest that the most massive galaxies have formed the bulk of their stellar population at earlier times and are essentially in place at redshift unity .
We investigate the influence of selection band and environment on the specific star formation rate ( SSFR ) .
We find that K -band selection indeed comes close to selection in stellar mass , while B -band selection purely selects galaxies in star formation rate .
We use a galaxy group catalogue constructed on the K -band selected MUNICS sample to study possible differences of the SSFR between the field and the group environment , finding a marginally lower average SSFR in groups as compared to the field , especially at lower redshifts .

The field-galaxy luminosity function in the B and R band as derived from the R -selected sample evolves out to z \simeq 2 in the sense that the characteristic luminosity increases but the number density decreases .
This effect is smaller at longer rest-frame wavelengths and gets more pronounced at shorter wavelengths .
Parametrising the redshift evolution of the Schechter parameters as M ^ { * } ( z ) = M ^ { * } ( 0 ) + a \ln ( 1 + z ) and \Phi ^ { * } ( z ) = \Phi ^ { * } ( 0 ) ( 1 + z ) ^ { b } we find evolutionary parameters a \simeq - 2.1 and b \simeq - 2.5 for the B band , and a \simeq - 1.4 and b \simeq - 1.8 for the R band .