  Arp 270 (NGC 3395 and NGC 3396) is the system of two actively star-forming
late-type galaxies in contact, which already have experienced at least one
close encounter in the past. We performed long-slit observations of peripheric
regions of this merging system with the 6-m telescope of SAO RAS. Line-of-sight
velocity distribution along the slits was obtained for gas and stellar
population. We found that the stellar component of NGC 3395 differs by its
velocity from the emission gas component in the extended region in the
periphery, which evidences a spatial separation of stars and gas in the tidally
disturbed galaxy. Gas abundances obtained by different methods demonstrate that
both galaxies are mildly underabundant (log(O/H) $\approx 8.4$) without
significant variations of metallicity along the slits. By comparing stellar and
gaseous masses of galaxies we came to conclusion that the chemical evolution of
gas is badly described by the closed box model. It allows us to admit that the
significant part of interstellar gas was swept out of galaxies during the
preceding encounter(s). A special attention was paid to the extended kpc-size
island of star formation between the galaxies. We have not found neither
noticeable kinematic decoupling of this region from the adjacent areas, nor any
peculiarities of its emission spectra, which evidences that it was formed
recently from the gas of NGC 3395 in the transition region between the
colliding galaxies.
