  It has been suggested that a trail of diffuse galaxies, including two dark
matter deficient galaxies (DMDGs), in the vicinity of NGC1052 formed because of
a high-speed collision between two gas-rich dwarf galaxies, one bound to
NGC1052 and the other one on an unbound orbit. The collision compresses the gas
reservoirs of the colliding galaxies, which in turn triggers a burst of star
formation. In contrast, the dark matter and pre-existing stars in the
progenitor galaxies pass through it. Since the high pressures in the compressed
gas are conducive to the formation of massive globular clusters (GCs), this
scenario can explain the formation of DMDGs with large populations of massive
GCs, consistent with the observations of NGC1052-DF2 (DF2) and NGC1052-DF4. A
potential difficulty with this `mini bullet cluster' scenario is that the
observed spatial distributions of GCs in DMDGs are extended. GCs experience
dynamical friction causing their orbits to decay with time. Consequently, their
distribution at formation should have been even more extended than that
observed at present. Using a semi-analytic model, we show that the observed
positions and velocities of the GCs in DF2 imply that they must have formed at
a radial distance of 5-10kpc from the center of DF2. However, as we
demonstrate, the scenario is difficult to reconcile with the fact that the
strong tidal forces from NGC1052 strip the extendedly distributed GCs from DF2,
requiring 33-59 massive GCs to form at the collision to explain observations.
