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).
Galaxy m-M $N_{\rm tot}$ $N_{\rm HST}$ $N_{<0.5 {\rm pc}}$ $L_{\rm HST}$/ $L_{>0.5 {\rm pc}}$
          V U
NGC 628 29.6 38 22 3 0.84 0.82
NGC 1156 29.5 22 21 5 0.85 0.86
NGC 1313 28.2 45 20 2 0.81 0.68
NGC 2835 28.9 9 8 6 0.20 0.17
NGC 2997 29.9 34 8 1 0.96 0.98
NGC 3184 29.5 13 9 3 0.79 0.83
NGC 3621 29.1 45 29 6 0.79 0.75
NGC 4258 29.47 44 26 2 0.91 0.91
NGC 5055 29.2 24 13 3 0.77 0.76
NGC 5194 29.6 69 33 2 0.99 0.99
NGC 5204 28.4 7 6 5 0.23 0.26
NGC 5236 27.9 149 29 9 0.79 0.82
NGC 5585 29.2 9 7 5 0.49 0.60
NGC 6744 28.5 18 4 0 1.00 1.00
NGC 6946 28.9 107 78 11 0.88 0.90
NGC 7424 30.5 10 6 0 1.00 1.00
NGC 7793 27.6 20 11 6 0.46 0.53


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