All Tables

Table 1: Fields identified by our ASTROVIRTEL program. The second column gives the exposure time that went into the coaddition (images with very bad PSF or seeing were rejected). Exposure times in parentheses indicate the total exposure time per association as identified by querator.
Table 2: GaBoDS data that was not taken by ourselves.
Table 3: All clumps except "C'' lie close to the peak of the track in Fig. 12, reducing the ambiguity in their redshift estimate.
Table 4: Fraction of blue galaxies. In the case of CL0056.03 a galaxy is defined to be "blue'' if V-R<0.755, i.e., if it lies more than $2\sigma$ below the cluster sequence $V-R=0.795\pm 0.02$ , as defined by galaxies with R<19. Galaxies with V-R>0.87 are exluded from the statistics. For CL0056.02 the $2\sigma$ -threshold for "blue'' galaxies is V-R<0.79. Galaxies with V-R>0.85 are excluded from the statistics. Note that the number of interlopers is reduced in the outer two annuli since they are significantly truncated by the edge of the field of view.
Table 5: Heliocentric redshifts for CL0056.03, taken from CHM98. Here, v denotes the radial velocity in $\rm{km~s^{-1}}$ together with its measurement errors $\sigma _v$ , and the index m indicates whether a galaxy is closer to the eastern cD galaxy ( ${\rm ID}=6$ ), or to the western one ( ${\rm ID}=16$ ).
Table 6: Properties for the eastern and western clumps around ${\rm cD_1}$ respectively ${\rm cD_2}$ .