  We have performed a spatially-resolved medium resolution long-slit
spectroscopy of a nearby E+A (post-starburst) galaxy system,
SDSSJ161330.18+510335.5. This E+A galaxy has an obvious companion galaxy 14kpc
in front with the velocity difference of 61.8 km/s. Both galaxies have
obviously disturbed morphology We have found that H$\delta$ equivalent width
(EW) of the E+A galaxy is greater than 7\AA galaxy wide (8.5 kpc). The E+A
galaxy have a weak [OIII] emission (EW$\sim$1\AA) by $\sim$2.6 kpc offset from
the peak of the Balmer absorption lines. We detected a rotational velocity in
the companion galaxy of $>$175km/s. The progenitor of the companion may have
been a rotationally-supported, but yet passive S0 galaxy. The age of the E+A
galaxy after quenching the star formation is estimated to be 100-500 Myr, with
its centre having slightly younger stellar population. These findings are
inconsistent with a simple picture where the dynamical interaction creates
infall of the gas reservoir that causes the central starburst/post-starburst.
Instead, our results present an important example where the galaxy-galaxy
interaction can trigger a galaxy-wide post-starburst phenomena.
