  We investigate the structural, kinematical, and spectrophotometric properties
of ``E+A'' galaxies -- those with strong Balmer absorption lines but no
significant [OII] emission -- using numerical simulations combined with stellar
population synthesis codes. We particularly focus on the two-dimensional (2D)
distributions of line-of-sight velocity, velocity dispersion, colors, line
index in E+A galaxies formed via the interaction and merging of two gas-rich
spirals. Our numerical simulations demonstrate that E+A elliptical galaxies
formed by major galaxy merging have positive radial color gradients and
negative radial H$\delta$ gradients by virtue of their central poststarburst
populations. Furthermore, we show that the projected kinematical and
spectroscopic properties of the simulated E+A galaxies can be remarkably
different for different major merger models. For example, the simulated E+A
ellipticals with kinematically decoupled cores clearly show regions of strong
H$\delta$ absorption which are very flattened, with differences in rotation and
velocity dispersion between the old and young stars. E+A ellipticals are highly
likely to show more rapid rotation and a smaller central velocity dispersion in
young stars than in old ones.We also provide specific predictions on the
structural, kinematical, and spectrophotometric properties of young globular
cluster systems in E+A's. Based on these results, we discuss the importance of
spatially resolved, integral field unit spectroscopy on large (8-10m)
ground-based telescopes in confirming the formation of kinematically distinct
cores in elliptical galaxies produced via dissipative merging and determining
the most probable physical mechanism(s) for E+A formation with disky and
spheroidal morphologies.
