  Recent observations revealed a mysterious ultra diffuse galaxy, NGC1052-DF2,
in the group of a large elliptical galaxy, NGC1052. Compared to expectations
from abundance matching models, the dark matter mass contained in NGC1052-DF2
is smaller by a factor of $\sim 400$. We utilize controlled $N$-body
simulations of the tidal interaction between NGC1052 and a smaller satellite
galaxy, that we suppose as the progenitor of NGC1052-DF2, to test if tidal
stripping can explain dark-matter deficiency at such levels. We find that when
assuming a tightly bound and quite radial orbit and cored density structure for
the dark halo of the satellite, our simulations reproduce well both the mass
profile and the effective radius inferred from the observations of NGC1052-DF2.
Orbital parameters are in the tail, but still consistent with measurements of
their distributions from cosmological simulations. Such strongly dark-matter
deficient galaxies, in our scenario, are thus expected to be relatively rare in
groups and clusters, and not present in the field.
