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

Globular clusters (GCs) are often used to estimate the dark matter content of galaxies, especially dwarf galaxies, where other kinematic tracers are lacking. These estimates typically assume spherical symmetry and dynamical equilibrium, assumptions that may not hold for the sparse GC population of dwarfs in galaxy clusters. We use a catalogue of GCs tagged on to the Illustris simulation to study the accuracy of GC-based mass estimates. We focus on galaxies in the stellar mass range 10(8)-10(11.8) M-circle dot identified in nine simulated Virgo-like clusters. Our results indicate that mass estimates are, on average, accurate in systems with GC numbers N-GC >= 10 and where the uncertainty of individual GC line-of-sight velocities is smaller than the inferred velocity dispersion, sigma(GC). In cases where N-GC <= 10, however, biases may result, depending on how sigma(GC) is computed. We provide calibrations that may help alleviate these biases in methods widely used in the literature. As an application, we find a number of dwarfs with - comparable with the ultra-diffuse galaxy NGC 1052-DF2 (DF2), notable for the low sigma(GC) of its 10 GCs - that have sigma(GO) similar to 7-15 kms(-1). These DF2 analogues correspond to relatively massive systems at their infall time (M-200 similar to 1-3 x 10(11) M-circle dot), which have retained only 3-17 GCs and have been stripped of more than 95 per cent of their dark matter. Our results suggest that extreme tidal mass loss in otherwise normal dwarf galaxies may be a possible formation channel for ultra-diffuse objects such as DF2.

Automated summary

The study found that using globular clusters (GCs) to estimate mass may result in biases in some cases, requiring calibration; some dwarf galaxies have GC velocity dispersion similar to the ultra-diffuse galaxy NGC 1052-DF2, suggesting extreme tidal mass loss as a possible formation channel for ultra-diffuse objects.