Dynamical Modeling of NGC 7252 and the Return of Tidal Material

Motivated by recent neutral hydrogen observations with the VLA, we have undertaken an investigation into the interaction that produced the well- known merger remnant NGC 7252. Through fully self-consistent N-body simulations, we are able to reproduce the kinematic character of the H I observations quite well, including the velocity reversals observed along each tidal tail. In the simulation these reversals arise from particles which have turned around in their orbit and are moving to smaller radii. The bases of the tails fall back quickly to small pericentric distances, while the more distant regions fall back more slowly to ever increasing pericentric distances. This delayed return of tidally ejected material may extend over many Gyr. The evolution of the merger is followed numerically for 800h^-1^ Myr beyond the best fit time. We find that nearly half of the present tail material, or of order 10^9^h^-2^ M_sun_ of neutral hydrogen and 2 x 10^9^ h^-2^ L_sun_ of starlight, will return to within 13h^-1^ kpc of the nucleus within this time span. While the collisionless stars of the tails will continue orbiting between their inner and outer turning points, the observations show the H I gas of the tails disappearing upon its return. We discuss this result in light of the lack of central H I in the main body of the merger remnant.