Halo mass estimates from the Globular Cluster populations of 175 Low
  Surface Brightness Galaxies in the Fornax Cluster
  The halo masses $M_{halo}$ of low surface brightness (LSB) galaxies are
critical measurements for understanding their formation processes. One
promising method to estimate a galaxy's $M_{halo}$ is to exploit the empirical
scaling relation between $M_{halo}$ and the number of associated globular
clusters ($N_{\mathrm{GC}}$). We use a Bayesian mixture model approach to
measure $N_{\mathrm{GC}}$ for 175 LSB ($23\leq\left\langle \mu_{e,r}
\right\rangle [\mathrm{mag\ arcsec}^{-2}]\leq 28$) galaxies in the Fornax
cluster using the Fornax Deep Survey (FDS) data; this is the largest sample of
low mass galaxies so-far analysed for this kind of study. The proximity of the
Fornax cluster means that we can measure galaxies with much smaller physical
sizes ($0.3\leq r_{e,r}\ [\mathrm{kpc}]\leq 9.5$) compared to previous studies
of the GC systems of LSB galaxies, probing stellar masses down to
$M_{*}\sim10^{5}\mathrm{M_{\odot}}$. The sample also includes \nudg\
ultra-diffuse galaxies (UDGs), with projected $r$-band half-light radii greater
than 1.5 kpc. Our results are consistent with an extrapolation of the
$M_{*}-M_{halo}$ relation predicted from abundance matching. In particular, our
UDG measurements are consistent with dwarf sized halos, having typical masses
between $10^{10}$ and $10^{11}\mathrm{M_{\odot}}$. Overall, our UDG sample is
statistically indistinguishable from smaller LSB galaxies in the same magnitude
range. We do not find any candidates likely to be as rich as some of those
found in the Coma cluster. We suggest that environment might play a role in
producing GC-rich LSB galaxies.
