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It is demonstrated that the kinematics of the 10 star clusters in NGC2052-DF2is compatible with a high dynamical mass close to those implied by the standardstellar-to-halo-mass ratio (SHMR). The analysis relies on a convenient form forthe distribution function (DF) of projected phase space data, capturingnon-gaussian features in the spread of true velocities of the mass tracers. Akey ingredient is tidal stripping by the gravity of the apparently nearbylarger galaxy, NGC 1052. Tidal stripping decreases the range of velocities ofmass tracers, while only mildly lowering the total mass inside the trimmingradius $r_{tr}$. The analysis is performed assuming halo profiles consistentwith simulations of the $\Lambda$CDM model. For the fiducial value $r_{tr}=10$kpc, we find that the virial mass of the pre-trimmed halo is $M<1.6\times10^{10}M_\odot$ at $2\sigma $ ($95\%$) and $M<8.6\times 10^{9}M_\odot$ at$1.64\sigma$ ($90\%$). For the mass within 10 kpc we obtain,$M_\mathrm{10kpc}<3.9\times 10^{9}M_\odot$ and $<2.9\times 10^{9}M_\odot$ at$2\sigma$ and $1.64\sigma$, respectively. The $2\sigma$ upper limit on thevirial mass is roughly a factor of 3-5 below the mean SHMR relation.Taking$r_{tr}=20$ kpc, lowers the $2\sigma$ virial mass limits by a factor of $\sim 4$, bringing our results closer to those of Wasserman et al. (2018) withouttheir SHMR prior.

Towards a higher mass for NGC1052-DF2: an analysis based on full distribution functions