  The discovery of NGC 1052-DF2 and subsequent modeling have shown that NGC
1052-DF2 is deficient in dark matter and is in conflict with the standard
stellar-to-halo mass ratio. In this work, we aim to resolve the degeneracy
between the dynamical models on the mass estimate of the NGC 1052-DF2.We
constructed mass models of NGC 1052-DF2 using an anisotropic distribution
function with a radially varying anisotropy parameter and studied the effect of
the various model parameters on the dark matter estimates. We used the observed
stellar photometry as an input parameter to construct the distribution function
and employed a Markov Chain Monte Carlo (MCMC) method to estimate the dark
matter model parameters.We find that mass models with a cuspy dark matter halo
have comparable $\chi^{2}$ to models with zero dark matter. Moreover, the cuspy
dark matter halo fails to consistently account for the observed velocity
dispersion in the inner and outer regions of the galaxy. Consequently, we rule
out the possibility of a cuspy dark matter halo for describing the mass models
of NGC 1052 - DF2. Our study shows that the cored dark matter halo model with a
total mass of $\log(M_{DM}/M_{\odot})=10.5$ explains the observed kinematics
but requires an extraordinarily large scale length (20kpc) and an outer cutoff
radius (26kpc). While the cored mass model provides a comparatively better fit,
our findings emphasize that the mass models are largely unconstrained by the
available kinematic data. Our results suggest that NGC 1052 - DF2 may not only
have an ultra-diffuse stellar distribution but that it can, within
uncertainties in the available kinematic data, potentially host an
ultra-diffuse dark matter distribution compatible with the standard
stellar-to-halo mass relation (SHMR) predicted by galaxy formation and
evolution models
