All Tables

Table 1: Summary of the differences of the object catalogs used for the lensing analyses of Erben et al. (2000) and this work. The brightness key refers to the magnitude bins used to split the sample (note that the magnitudes are not calibrated).
Table 2: Overview of the $M_{\rm ap}$ values and signal-to-noise ratios of the peaks found in the analyses of the CFHT data. We also give the number of galaxies located in the aperture (N), and the (weighted) average galaxy ellipticity dispersion $\sigma _{\varepsilon }$ , as well as the offset to the assumed centroid position, measured in the sky coordinate system. In two cases, there was no $M_{\rm ap}$ peak in the vicinity of the dark clump - we then quote the values at the reference position (in italics).
Table 3: Overview of the $M_{\rm ap}$ values and signal-to-noise ratios of the peaks found in the analyses of the HST data. We also give the number of galaxies located in the aperture (N), and the (weighted) average galaxy ellipticity $\sigma _{\varepsilon }$ , as well as the offset to the assumed centroid position, measured in the sky coordinate system. For the smallest filter scale ( $80 \hbox {$^{\prime \prime }$ }$ ), the anlysis of all galaxies yields two peaks in the vicinity of the dark clump position, both of which are listed. For the medium bright bin, there is no peak close to the dark clump in the largest two filter scales - we then quote the values at the reference position (in italics).
Table B.1: Overview of the $M_{\rm ap}$ analyses discussed in this appendix. Shown are the results at the position of the dark clump as measured in the ground-based data, since we want to determine the cause of the high $M_{\rm ap}$ amplitude in the ground-based data at this position. We list the ellipticity dispersion, the $M_{\rm ap}$ value itself, and the signal-to-noise ratio. For those analyses of the 350 matched objects, we give both the results of using the ground-based and of using the space-based data. For the second block from the bottom of the table, the ground-based analysis uses the space-based weights and vice versa. For the last block, the ${\varepsilon _1}$ component of the HST measurements is modified by applying the inverse of the linear fit between space-based and ground-based ellipticities. Evaluating $M_{\rm ap}$ only at the ground-based dark clump position biases the result in favor of larger ground-based values. For a better comparison of the general values, we quote the highest significance found in the vicinity of this position in parentheses.