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tokens: is whether or not the GCS from NGC 1275 itself is contributing to the NGC 1272 totals particularly in ACS-3. From the NGC 1275 profile (see comments below and the lower panel of Figure 8 ), it appears that the contribution from NGC 1275 at the kpc projected distance of NGC 1272 will be at the level of only a few percent. If and when more complete imaging coverage of the core Perseus region is available, it will be possible to solve for the spatial distributions of both galaxies simultaneously and more accurately (see e.g., Wehner et al. 2008 , for an example in the Hydra cluster). For the central giant NGC 1275, the available material is much more limited and the conclusions about total GC population correspondingly rougher. We use field ACS-1 along with ACS-6 to set the local background, though here we are forced to assume that is roughly constant over the region concerned. The measurements are shown in the lower panel of Figure 8 , replotted from Figure 6 . The combination of this radial profile and the inner data from Penny et al. ( 2012 ) indicates that from outward, and is relatively flat inside 60′′. The main concerns in estimating its total population are the true local background level, and how far outward the NGC 1275 halo extends before fading into the ICM; the present data do not answer either of these satisfactorily. Here we simply use an outer radius (100 kpc) for integration of the profile and arcsec −2 as above. The result is then GCs for , not including any (unknown) systematic error in the adopted background. Extrapolating over all magnitudes as described above gives N GC = 13,500 ± 2000 and a specific frequency , including ±0.1 mag uncertainties in the GCLF turnover and dispersion as above. This total GC population and S N would make NGC 1275 quite similar to M87 in Virgo (e.g., Harris 2009b ). We emphasize once again that a better assessment will require a wider-field survey in which the GC populations in the member galaxies, and the IGCs, can both be determined more completely. Nevertheless, this very limited imaging material is enough to suggest that both of the dominant Perseus galaxies appear to have very populous GC systems. The closest analogy may be the more well known Coma cluster, where both NGC 4874 and 4889 have similarly large GC populations but where the central cD (NGC 4874) has the higher specific frequency. 5. Discussion: The IGC Population The data discussed in this paper consist of only 11 pencil-beam probes of the GC population, and thus fall far short of a genuine wide-field survey of the Perseus cluster. Only a more comprehensive survey to similar depth will be able to address the true spatial distribution of the IGCs and their total number. Nevertheless, we can make a very rough attempt to gauge the total GC population. We assume, following Figures 6 and 8 , that σ (IGC) is approximately constant at arcsec −2 in the inner part of the cluster and then falls off as further out. The inflection point