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tokens: parameter being set using equation (8) of Dutton Macciò ( 2014 ). When using this method for NFW profiles, we do not correct the concentration parameter from that of Dutton Macciò ( 2014 ) as is done for Di Cintio et al. ( 2014 ) profiles. Figure 9. A comparison of the halo mass estimate from GCs and the dynamical mass estimates for VCC 1287. We plot the Beasley et al. ( 2016 ) GC tracer mass estimate (circle) and our stellar velocity dispersion dynamical mass measurement (star). A total halo mass estimate based on the GC number–halo mass relation of Burkert Forbes ( 2020 ) is plotted using two differing assumptions of halo profile (blue region – NFW cusp profile; red region – Di Cintio et al. 2014 halo core profile). For both dynamical mass measurements to be consistent with the halo mass estimate from the number of GCs ( N GC = 22 ± 8; Beasley et al. 2016 ), either a lower halo concentration parameter or the presence of a dark matter core is required. Theoretical efforts to simulate the formation of UDGs frequently rely either on the creation of a cored dark matter profile (e.g. Di Cintio et al. 2017 ) or on its pre-existence (e.g. Carleton et al. 2019 ). Jiang et al. ( 2019 ) also found UDGs in the nihao simulation to lie in cored dark matter profiles along with having concentration parameters lower than that expected based on dwarf galaxy and L * galaxy control samples. It is yet to be established whether these low concentration parameters are the cause of, or result of, UDG formation (Jiang et al. 2019 ). In both, the case of a cored halo or one with a lower concentration parameter, the enclosed mass of the profile would be biased towards lower values, causing NFW profiles to represent an upper limit to the enclosed mass. For this reason, we also choose to include the Di Cintio et al. ( 2014 ) halo profile as these models naturally produce cores, which may be more representative of the actual profile of UDGs. There exists a slight tension between the dynamical masses and the halo mass, as plotted, calculated with the Burkert Forbes ( 2020 ) relation. This tension may be the result of incorrect assumptions made in converting observations into dynamical masses or, more likely, incorrect halo profile assumptions made in plotting for the full halo mass inferred from GC counts (e.g. VCC 1287 may have a lower concentration parameter than we calculate with Dutton Macciò 2014 ). In order for the dynamical mass measurements to be consistent with the halo mass estimate from the Burkert Forbes ( 2020 ) relation, the dark matter halo of VCC 1287 must either be cored (e.g. the Di Cintio et al. 2014 profile of Fig. 9 ) or have a low-concentration parameter. We note that the total halo mass from the Burkert Forbes ( 2020 ) relation implies a halo more massive than what is expected from the stellar mass–halo mass relation similar to other UDGs in the Coma Cluster (Forbes et al. 2020 ). Indeed, both the stellar mass and GC system richness of VCC