tokens: 9799, the total population of GCs out to (the limit of the ACS field of view, as well as the limit of the halo-light photometry) is brighter than I = 27.0 from integration of the radial profile. This limit is 0.12 mag fainter than the GCLF peak (Paper I) and thus should include 54% of the total over all luminosities assuming the GCLF is Gaussian in number per unit magnitude, and using the parameters from Paper I. We therefore obtain for (110 kpc). Integrating the light profile (Seigar et al. 2007 ) to the same radius gives a total integrated magnitude , which corresponds to assuming a mean color for giant early-type galaxies. The specific frequency of the GC system is then . If we were to choose to integrate the entire GC system profile all the way to the WFC3 field at R = 300 kpc, the result would be clusters, but this estimate is much more uncertain. For UGC 10143, if again we restrict the calculation conservatively to the ACS field of view (), the total number of GCs with is , which translates into over all magnitudes. Integration of the halo light (Donzelli et al. 2011 ) into the same radius gives , . Finally then, to that radius. The more risky extrapolation of the GC profile out to the WFC3 field limit at (270 kpc) would give . The UGC 9799 GC system is therefore relatively richer than for UGC 10143, but the specific frequencies of both are in the range observed for other BCGs (e.g., Harris et al. 2013 ). For NGC 4889, the profile integration gives clusters brighter than (); this limiting magnitude is very near the GCLF peak point. We therefore double that number to , which when combined with gives a specific frequency of . This galaxy is very luminous, but relative to its size, it does not have an exceptionally populous cluster system in the more typical BCG range. The story is somewhat different and more complex for the central Coma cD NGC 4874: Peng et al. ( 2011 ) estimate GCs excluding the more extended IGC population. When we use , as did Harris et al. ( 2009 ), we obtain . If instead N tot is normalized to the entire luminosity profile out to a much larger radius of 520 kpc, then S N decreases markedly to 3.7 ± 0.1 (Peng et al. 2011 ); but since the IGC clusters outnumber the “intrinsic” GCs that are more clearly associated with the galaxy itself, this lower specific frequency is perhaps more of a statement about S N (IGC). In this respect, it is worth noting that Durrell et al. ( 2014 ) find for the Virgo cluster GCs in their entirety, of which a large fraction are IGCs, and less than a quarter are from M87 itself. 8. DISCUSSION For extremely broad and nearly featureless MDFs such as we find in NGC 6166 (Paper II), UGC 9799, and UGC 10143, the imposition of a bimodal Gaussian numerical model, or any simplistic multimodal fitting process, begins to look increasingly arbitrary. Transformation of their CDFs back into the underlying metallicity distribution by way of Equation ( 1 ) yields a similarly broad unimodal MDF. We stress
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