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[Abridged] We perform on galaxy mock catalogues the same colour-densityanalysis made by Cucciati et al. (2006) on a 5 Mpc/h scale using the VVDS-Deepsurvey, and compare the results from mocks with observed data. We use mockswith the same flux limits (I=24) as the VVDS (CMOCKS), built using the semi-analytic model by De Lucia & Blaizot (2007) applied to the MillenniumSimulation. From CMOCKS, we extracted samples of galaxies mimicking the VVDSobservational strategy (OMOCKS). We computed the B-band Luminosity Function LFand the colour-density relation (CDR) in the mocks. We find that the LF inmocks roughly agrees with the observed LF, but at z<0.8 the faint-end slope ofthe model LF is steeper than the VVDS one. Computing the LF for early and latetype galaxies, we show that mocks have an excess of faint early-type and ofbright late-type galaxies with respect to data. We find that the CDR in OMOCKSis in excellent agreement with the one in CMOCKS. At z~0.7, the CDR in mocksagrees with the VVDS one (red galaxies reside mainly in high densities). Yet,the strength of the CDR in mocks does not vary within 0.2<z<1.5, while theobserved relation flattens with increasing z and possibly inverts at z=1.3. Weargue that the lack of evolution in the CDR in mocks is not due only toinaccurate prescriptions for satellite galaxies, but that also the treatment ofcentral galaxies has to be revised. The reversal of the CDR can be explained bywet mergers between young galaxies, producing a starburst event. This should beseen on group scales. A residual of this is found in observations at z=1.5 onlarger scales, but not in the mocks, suggesting that the treatment of physicalprocesses affecting satellites and central galaxies in models should berevised.

Comparison of the VIMOS-VLT Deep Survey with the Munich semi-analytical model. II. The colour-density relation up to z=1.5