All Tables

Table 1: The four VVDS galaxy types.
Table 2: Measurement of the clustering length for galaxy subsamples ranging from z=0.2 to z=2, letting the slope $\gamma$ free or fixing the slope to the average value measured for a given type. The absolute M_{B_AB} magnitude and number of objects are indicated.
Table 3: Relative bias between early-type and late-type galaxies (from spectral type classification), and "red'' vs. "blue'' galaxies (separated using the color bi-modality).
Table 4: Number of galaxies and mean B rest-frame absolute magnitude (h=1) of the sample separated using the color bimodality. The number of "red'' and "blue'' galaxies classified as early (T1&2) and late (T3&4) spectral types are identified. We note that the populations of "red'' and T1&2 as well as the populations of "blue'' and T3&4 galaxies are mostly the same, except for a significant cross-over population which could explain the observed difference in clustering (see text).
Table 5: Measurements of the clustering length and slope for galaxy subsamples divided following the color bimodality.