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Using a new method to estimate total galaxy mass (M$_{\rm T}$) and twosamples of low luminosity galaxies containing measurements of the number ofglobular clusters (GCs) per galaxy (N$_{\rm GC}$), we revisit the N$_{\rmGC}-$M$_{\rm T}$ relation using a total of 203 galaxies, 157 of which haveM$_{\rm T}$ $\ \le 10^{10}$ M$_\odot$. We find that the relation is nearlylinear, N$_{\rm GC} \propto$ M$_{\rm T}^{0.92\pm0.08}$ down to at least M$_{\rmT} \sim 10^{8.75}$ M$_\odot$. Because the relationship extends to galaxies thataverage less than one GC per galaxy and to a mass range in which mergers arerelatively rare, the relationship cannot be solely an emergent property ofhierarchical galaxy formation. The character of the radial GC distribution inlow mass galaxies, and the lack of mergers at these galaxy masses, also appearsto challenge models in which the GCs form in central, dissipativelyconcentrated high-density, high-pressure regions and are then scattered tolarge radius. The slight difference between the fitted power-law exponent and avalue of one, leaves room for a shallow M$_{\rm T}$-dependent variation in themean mass per GC that would allow the relation between total mass in GCs andM$_{\rm T}$ to be linear.

Revisiting the relation between the number of globular clusters and galaxy mass for low mass galaxies