The properties of the merger remnant in this experiment are rather different from those found in other simulations of merging groups. Weil and Hernquist's (1996) simulations produced remnants which are nearly oblate with a small flattening. They also have a modest amount of rotational support about their minor axes. These results contrast with the prolate nearly non-rotating object in the cluster simulation. The differences can be attributed to initial conditions. The group simulations start with galaxies on random trajectories selected from an isotropic distribution while the cosmological mergers are strongly anisotropic because of the initial filamentary structure. The initial isotropy leads to a rounder, oblate remnant while collapse down a filament appears to lead to a prolate, elongated object.