  The paper presents results of studying the kinematics of the ionized gas in
the galaxy of the Large Magellanic Cloud type NGC 7292 obtained with the 2.5-m
telescope of the Caucasian Mountain Observatory (CMO SAI MSU) and the 6-m BTA
telescope of the Special Astrophysical Observatory (SAO RAS). Analysis of the
velocity fields of the ionized and neutral hydrogen showed that the kinematic
center of NGC 7292 located at the center of the bar, northwest of the
photometric center of the galaxy (the southeastern end of the bar) previously
taken as the center of NGC 7292. In addition to the circular rotation of the
gas, the radial motions associated with the bar play a significant role in the
kinematics of the disk. The observed perturbations of the gaseous-disk
kinematics induced by the ongoing star formation do not exceed those caused by
the bar. It is possible that part of the non-circular motions (at the
southeastern end of the bar which is the brightest HII region) may be related
to the effects of the capture of a dwarf companion or a gaseous cloud.
