  Merger remnants of small groups of galaxies are contrasted with relics of
mergers of pairs of galaxies to determine which process produces objects that
best compare to real ellipticals. In both cases, the progenitors consist of
self-gravitating disks, halos, and, sometimes, bulges. Pairs of galaxies merge
from orbits that initially have zero--energy. The systems that produce multiple
merger remnants are dense, six--member groups in virial equilibrium with low
velocity dispersions. Multiple and pair mergers produce remnants which differ
in both their spatial and kinematic properties. Multiple merger remnants have
small triaxialities and are most likely to appear nearly round from most
viewing angles. They possess cores, with sizes of a few tenths of an effective
radius, that are more extended than pair remnant cores, even when bulges are
included in the progenitors. In multiple mergers, the spin of all components --
halo, disk, and bulge -- increases and, while velocity dispersion dominates in
the central regions, $v_r/\sigma \approx 1$ outside an effective radius in some
projections. The angular momentum and minor axis vectors are aligned for
multiple merger remnants. During merging of multiple progenitors, about half of
the orbital angular momentum in each luminous component is converted into
internal rotation in that component. Material is prevented from accumulating in
the center of multiple merger remnants as efficiently as it does in pair
mergers. In pair mergers that include gas, unrealistically steep surface
brightness profiles have been produced in center of the remnants; in multiple
mergers the formation of overdense nuclei may be impeded, thus allowing more
successful comparison with real elliptical galaxies.
