All Tables

Table 1: The coordinates of the four fields investigated so far, and the number of galaxies per field, $I\leq 23$ and $0.2\leq z\leq 1.07$ , also given is the number of bright galaxies ( $M_B<-18+5 \log h$ ) in this redshift and apparent magnitude range.
Table 2: The measured amplitude of the projected correlation function in different redshift intervals, at $r_{\rm p}\approx316 ~h^{-1}$ kpc for CADIS and at $r_{\rm p}\approx500 ~h^{-1}$ kpc for the LCRS (first lines), respectively, the integral constraint ${\cal I}$ and $\xi_{1{\rm ~Mpc}}$ as calculated from the ${\cal I}$ -corrected amplitudes of $w(r_{\rm p})$ , for different world models. Numbers in italic indicate that this values are inferred from the LCRS.
Table 3: The measured amplitude of the projected correlation function at $r_{\rm p}\approx316 ~h^{-1}$ kpc for the bright ( $M_B\leq-18+5 \log h$ ) galaxies, the integral constraint ${\cal I}$ , and $\xi_{1{\rm ~Mpc}}$ , calculated from the ${\cal I}$ -corrected A, for different world models. Note that for the bright sample the calculation for the first redshift bin was started at z=0.25 instead of z=0.2, because there are only very few bright galaxies at redshifts smaller than 0.3.
Table 4: The measured amplitude of the projected correlation function at $r_{\rm p}=316 ~h^{-1}$ kpc and the integral constraint ${\cal I}$ , in different redshift intervals for two SED bins, for different world models.
Table 5: The amplitudes of the three-dimensional correlation function $\xi (r)$ at a comoving distance of r=1 Mpc, for red ( $SED\leq 60$ ) and blue (SED>60) galaxies; the integral constraint has been taken into account in the calculation.
Table 6: The parameter q for early type ( $SED\leq 60$ ) galaxies, for a fit done without taking the the LCRS point into account, and for a fit including it. The evolution of the bright sample is shown for comparison.