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The goal of this work is to probe the total mass distribution of early-typegalaxies with globular clusters (GCs) as kinematic tracers, by constraining theparameters of the profile with a flexible modelling approach. To that end, weleverage the extended spatial distribution of GCs from the SLUGGS survey($\langle R_{\rm GC,\ max} \rangle \sim 8R_{\rm e}$) in combination withdiscrete dynamical modelling. We use discrete Jeans anisotropic modelling incylindrical coordinates to determine the velocity moments at the location ofthe GCs in our sample. We use a Bayesian framework to determine the best-fitparameters of the total mass density profile and orbital properties of the GCsystems. We find that the orbital properties (anisotropy and rotation of thedispersion-dominated GC systems) minimally impact the measurements of the innerslope and enclosed mass, while a strong presence of dynamically-distinctsubpopulations or low numbers of kinematic tracers can bias the results. Owingto the large spatial extent of the tracers our method is sensitive to theintrinsic inner slope of the total mass profile and we find $\overline{\alpha}= -1.88\pm 0.01$ for 12 galaxies with robust measurements. To compare ourresults with literature values we fit a single power-law profile to theresulting total mass density. In the radial range 0.1-4~$R_{\rm e}$ ourmeasured slope has a value of $\langle \gamma_{\rm tot}\rangle = -2.22\pm0.14$and is in good agreement with the literature.

Total mass slopes and enclosed mass constrained by globular cluster system dynamics