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This paper presents an analysis of the correlation between the number ofglobular clusters (N_GC) in giant galaxies and the mass of the galaxies'central supermassive black hole (M_SMBH). I construct a sample of 20elliptical, spiral, and S0 galaxies with known SMBH masses and withaccurately-measured globular cluster system properties derived from wide-fieldimaging studies. The coefficients of the best-fitting N_GC-M_SMBH relation forthe early-type galaxies are consistent with those from previous work but insome cases have smaller relative errors. I examine the correlation between N_GCand M_SMBH for various subsamples and find that elliptical galaxies show thestrongest correlation while S0 and pseudobulge galaxies exhibit increasedscatter. I also compare the quality of the fit of the numbers of metal-poorglobular clusters versus SMBH mass and the corresponding fit for metal-richglobular clusters. I supplement the 20-galaxy sample with ten additionalgalaxies with reliable N_GC determinations but without measured M_SMBH. I usethis larger sample to investigate correlations between N_GC and host galaxyproperties like total galaxy luminosity and stellar mass and bulge luminosityand mass. I find that the tightest correlation is between N_GC and total galaxystellar mass. This lends support to the notion that N_GC and M_SMBH are notdirectly linked but are correlated because both quantities depend on the hostgalaxy potential. Finally, I use the N_GC-M_SMBH relation derived from the20-galaxy sample to calculate predicted M_SMBH values for the ten galaxies withaccurate N_GC measurements but without measured SMBH masses.

Exploring the Correlations between Globular Cluster Populations and Supermassive Black Holes in Giant Galaxies