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The halo masses $M_{halo}$ of low surface brightness (LSB) galaxies arecritical measurements for understanding their formation processes. Onepromising method to estimate a galaxy's $M_{halo}$ is to exploit the empiricalscaling relation between $M_{halo}$ and the number of associated globularclusters ($N_{\mathrm{GC}}$). We use a Bayesian mixture model approach tomeasure $N_{\mathrm{GC}}$ for 175 LSB ($23\leq\left\langle \mu_{e,r}\right\rangle [\mathrm{mag\ arcsec}^{-2}]\leq 28$) galaxies in the Fornaxcluster using the Fornax Deep Survey (FDS) data; this is the largest sample oflow mass galaxies so-far analysed for this kind of study. The proximity of theFornax cluster means that we can measure galaxies with much smaller physicalsizes ($0.3\leq r_{e,r}\ [\mathrm{kpc}]\leq 9.5$) compared to previous studiesof 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 greaterthan 1.5 kpc. Our results are consistent with an extrapolation of the$M_{*}-M_{halo}$ relation predicted from abundance matching. In particular, ourUDG measurements are consistent with dwarf sized halos, having typical massesbetween $10^{10}$ and $10^{11}\mathrm{M_{\odot}}$. Overall, our UDG sample isstatistically indistinguishable from smaller LSB galaxies in the same magnituderange. We do not find any candidates likely to be as rich as some of thosefound in the Coma cluster. We suggest that environment might play a role inproducing GC-rich LSB galaxies.

Halo mass estimates from the Globular Cluster populations of 175 Low Surface Brightness Galaxies in the Fornax Cluster