All Tables

Table 1: Exposures. $\Delta (\alpha ,\delta )$ indicates the offsets in right ascension and declination between the coordinate systems of the WFPC2 frames and the ground-based data (tied to the USNO catalogue). The offsets are given in s/15 for right ascension and in arcseconds for declination (i.e. the $\cos\delta$ factor has not been applied to convert the offsets in $\alpha$ to true arcsecs).
Table 2: Explanation of comment codes.
Table 3: All clusters with S/N>50 on HST images. Photometry is from ground-based data while morphological data are from HST/WFPC2 images. The first 10 rows of the table are reproduced here; the full table (1358 rows) is only available in electronic form at the CDS.
Table 4: Additional comments (only 5 sample entries given).
Table 5: HST photometry for the same clusters listed in Table 3. All magnitudes are in the STMAG system, measured in a $0\hbox{$.\!\!^{\prime\prime}$ }5$ aperture and applying an aperture correction of -0.2 mag. No corrections for foreground reddening have been applied. Only the first 10 rows are reproduced here.
Table 6: Tests of the ISHAPE profile-fitting algorithm. For each combination of input parameters ( V=20/21/22, FWHM =1 pc/2 pc) the output fitted FWHM and $\alpha$ parameters are shown for three initial guesses of $\alpha$ ( $\alpha _0 = 1.0/1.5/2.0$ ). Numbers in parentheses denote the object-to-object rms deviation around the mean values, excluding the two most deviating points at each extreme.
Table 7: Clusters from ground-based survey reidentified in HST images. Photometry is from ground-based data. FWHM is the full-width-at-half-maximum in pc derived from EFF $\alpha =1.5$ fits. The first 10 rows of the table are reproduced here; the full table (330 rows) is only available in electronic form at the CDS.
Table 8: Contamination of ground-based sample for individual galaxies. $N_{\rm tot}$ is the total number of cluster candidates identified in the ground-based surveys, $N_{\rm HST}$ is the subset of those candidates covered by HST images and $N_{<0.5 {\rm pc}}$ is the number of unresolved sources. The adopted distance moduli are also listed (see Paper I for references).
Table 9: Mean FWHM and effective radii for clusters in galaxies.
Table 10: Statistics on comment flags in different age intervals.