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Globular clusters (GCs) are often used to estimate the dark matter content ofgalaxies, especially dwarfs, where other kinematic tracers are lacking. Theseestimates typically assume spherical symmetry and dynamical equilibrium,assumptions that may not hold for the sparse GC population of dwarfs in galaxyclusters. We use a catalog of GCs tagged onto the Illustris simulation to studythe accuracy of GC-based mass estimates. We focus on galaxies in the stellarmass range 10$^{8} - 10^{11.8}$ M$_{\odot}$ identified in $9$ simulatedVirgo-like clusters. Our results indicate that mass estimates are, on average,quite accurate in systems with GC numbers $N_{\rm GC} \geq 10$ and where theuncertainty of individual GC line-of-sight velocities is smaller than theinferred velocity dispersion, $\sigma_{\rm GC}$. In cases where $N_{\rm GC}\leq 10$, however, biases may result depending on how $\sigma_{\rm GC}$ iscomputed. We provide calibrations that may help alleviate these biases inmethods widely used in the literature. As an application, we find a number ofdwarfs with $M_{*} \sim 10^{8.5}\, M_{\odot}$ (comparable to the ultradiffusegalaxy DF2, notable for the low $\sigma_{GC}$ of its $10$ GCs) with$\sigma_{\rm GC} \sim 7$ - $15\; \rm km \rm s^{-1}$. These DF2 analogscorrespond to relatively massive systems at their infall time ($M_{200} \sim 1$- $3 \times 10^{11}$ $M_{\odot}$) which have retained only $3$-$17$ GCs andhave been stripped of more than 95$\%$ of their dark matter. Our resultssuggest that extreme tidal mass loss in otherwise normal dwarf galaxies may bea possible formation channel for ultradiffuse objects like DF2.

Globular clusters as tracers of the dark matter content of dwarfs in galaxy clusters