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We have performed spatially resolved medium resolution long‐slit spectroscopy of a nearby E+A (post‐starburst) galaxy system, SDSS J161330.18+510335.5, with the FOCAS spectrograph mounted on the Subaru Telescope. This E+A galaxy has an obvious companion galaxy 14 kpc in front with the velocity difference of 61.8 km s −1 . Both galaxies have obviously disturbed morphology. Thus, this E+A system provides us with a perfect opportunity to investigate the relation between the post‐starburst phenomena and galaxy–galaxy interaction.  We have found that the Hδ equivalent width (EW) of the E+A galaxy is greater than 7 Å galaxy wide (8.5 kpc) with no significant spatial variation. The E+A galaxy has a weak [O  iii ] emission (EW ∼ 1 Å) offset by  ∼2.6 kpc  from the peak of the Balmer absorption lines. We detected a rotational velocity in the companion galaxy of &gt;175 km s −1 . The progenitor of the companion may have been a rotationally supported, but yet passive S0 galaxy. We did not detect significant rotation on the E+A galaxy. A metallicity estimate based on the   r − H   colour suggests   Z = 0.008  and 0.02, for the E+A and the companion galaxies, respectively. Assuming these metallicity estimates, the age of the E+A galaxy after quenching the star formation is estimated to be 100–500 Myr, with its centre having a slightly younger stellar population. The companion galaxy is estimated to have an older stellar population of &gt;2 Gyr of age with no significant spatial variation.  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 phenomenon.

Spatially resolved medium resolution spectroscopy of an interacting E+A (post‐starburst) system with the Subaru Telescope ★