Revisiting the relation between the number of globular clusters and
  galaxy mass for low mass galaxies
  Using a new method to estimate total galaxy mass (M$_{\rm T}$) and two
samples of low luminosity galaxies containing measurements of the number of
globular clusters (GCs) per galaxy (N$_{\rm GC}$), we revisit the N$_{\rm
GC}-$M$_{\rm T}$ relation using a total of 203 galaxies, 157 of which have
M$_{\rm T}$ $\ \le 10^{10}$ M$_\odot$. We find that the relation is nearly
linear, N$_{\rm GC} \propto$ M$_{\rm T}^{0.92\pm0.08}$ down to at least M$_{\rm
T} \sim 10^{8.75}$ M$_\odot$. Because the relationship extends to galaxies that
average less than one GC per galaxy and to a mass range in which mergers are
relatively rare, the relationship cannot be solely an emergent property of
hierarchical galaxy formation. The character of the radial GC distribution in
low mass galaxies, and the lack of mergers at these galaxy masses, also appears
to challenge models in which the GCs form in central, dissipatively
concentrated high-density, high-pressure regions and are then scattered to
large radius. The slight difference between the fitted power-law exponent and a
value of one, leaves room for a shallow M$_{\rm T}$-dependent variation in the
mean mass per GC that would allow the relation between total mass in GCs and
M$_{\rm T}$ to be linear.
