You can lose some of the cluster members if the faint end of the bin starts to go beyond the limiting magnitude of this field. As can be seen from the data, most clusters cease to be if the characteristic magnitude is moved at all. This is the number of galaxies found in the aperture within the 2 magnitude bin around the characteristic magnitude and then adjusted by the cluster percentage of aperture area common to the WFPC2 frame. This number was determined in a first pass of the algorithm by centering on all objects and building a table of limits as function of cluster bin and confidence level. A first pass of the algorithm built up a statistical sample of just what constitutes an overdensity in the MDS data.
Confidence levels are a function of the cluster bin.
This is a photometric redshift taken from the central bulge galaxy using the F814W and F606W filters. If only one of the F814W or F606W were present or if the v-band filter was F555W, then a mean galaxy color of 1 was used. For undetermined redshifts 9.99 was used as a dummy value. A 1.0 is a pure bulge cluster and conversely a 0.0 is a pure disk cluster. With few exceptions, the clusters are generally more bulgy than the average collection of galaxies in this cluster bin.