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We aim to explore the relationship between globular cluster total number,$N_{\rm GC}$, and central black hole mass, $M_\bullet$, in spiral galaxies, andcompare it with that recently reported for ellipticals. We present results forthe Sbc galaxy NGC 4258, from Canada France Hawaii Telescope data. Thanks towater masers with Keplerian rotation in a circumnuclear disk, NGC 4258 has themost precisely measured extragalactic distance and supermassive black hole massto date. The globular cluster (GC) candidate selection is based on the ($u^*\-\ i^\prime$) vs. ($i^\prime\ -\ K_s$) diagram, which is a superb tool todistinguish GCs from foreground stars, background galaxies, and young stellarclusters, and hence can provide the best number counts of GCs from photometryalone, virtually free of contamination, even if the galaxy is not completelyedge-on. The mean optical and optical-near infrared colors of the clusters areconsistent with those of the Milky Way and M 31, after extinction is taken intoaccount. We directly identify 39 GC candidates; after completeness correction,GC luminosity function extrapolation and correction for spatial coverage, wecalculate a total $N_{\rm GC} = 144\pm31^{+38}_{-36}$ (random and systematicuncertainties, respectively). We have thus increased to 6 the sample of spiralgalaxies with measurements of both $M_\bullet$ and $N_{\rm GC}$. NGC 4258 has aspecific frequency $S_{\rm N} = 0.4\pm0.1$ (random uncertainty), and isconsistent within 2$\sigma$ with the $N_{\rm GC}$ vs. $M_\bullet$ correlationfollowed by elliptical galaxies. The Milky Way continues to be the only spiralthat deviates significantly from the relation.

The relation between globular cluster systems and supermassive black holes in spiral galaxies. The case study of NGC 4258