  It is demonstrated that the kinematics of the 10 star clusters in NGC2052-DF2
is compatible with a high dynamical mass close to those implied by the standard
stellar-to-halo-mass ratio (SHMR). The analysis relies on a convenient form for
the distribution function (DF) of projected phase space data, capturing
non-gaussian features in the spread of true velocities of the mass tracers. A
key ingredient is tidal stripping by the gravity of the apparently nearby
larger galaxy, NGC 1052. Tidal stripping decreases the range of velocities of
mass tracers, while only mildly lowering the total mass inside the trimming
radius $r_{tr}$. The analysis is performed assuming halo profiles consistent
with 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 $M<1.6\times
10^{10}M_\odot$ 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 the
virial 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) without
their SHMR prior.
