  We have investigated the dependence of galaxy clustering on their intrinsic
luminosities at z ~ 1, using the data from the First Epoch VIMOS-VLT Deep
Survey (VVDS). We have measured the projected two-point correlation function of
galaxies, w_p(r_p), for a set of volume-limited samples at an effective
redshift <z>=0.9 and median absolute magnitude -19.6< M_B < -21.3. We find that
the clustering strength is rising around M_B^*, apparently with a sharper turn
than observed at low redshifts. The slope of the correlation function is
observed to steepen significantly from \gamma=1.6^{+0.1}_{-0.1} to
\gamma=2.4^{+0.4}_{-0.2}. This is due to a significant change in the shape of
w_p(r_p), increasingly deviating from a power-law for the most luminous
samples, with a strong upturn at small (< 1-2 h^{-1} Mpc) scales. This trend,
not observed locally, also results in a strong scale dependence of the relative
bias, b/b* and possibly imply a significant change in the way luminous galaxies
trace dark-matter halos at z ~ 1 with respect to z ~ 0.
