At this stage in the research our immediate goal has been to determine the relative metallicity of the cluster to standard sequences, rather than determining the absolute metallicity. To this end, the photometric indices, hk and m1, have been examined as they are both sensitive to the metallicity. It should be noted, however, that the hk index is more sensitive to the metallicity than the m1 index, and so can provide a better gauge for measuring the metallicity. We look at the dispersion or spread in the hk and m1 vs. color diagrams in both the vertical and horizontal directions in order to ascertain the effects from reddening on these photometric indices. There is a need for us to remove any non- members and binaries from the cluster data before we are able to truly consider the effects of reddening in the cluster. Looking to Figures 2 and 3, we do see that the expected trends in the hk, m1 color plots are indeed present. For these figures, the data used is limited to stars with index errors of ± 0.03 or less. In a perfect world, these plots would conform to well-defined curves. The preliminary results we have gathered thus far do show some broadening in the hk and even m1 indices, but it is too early to ascertain whether or not this is due to reddening. This is due to the incompleteness of the data sets we have used in our diagrams