disk $z_{0}$ is approximately twice as large as at the center). Such stellar disk structure is expected for the galaxies subjected to strong external accretion or merging (Toth & Ostriker 1992, Quinn et al. 1993).

The rotation curve of NGC 3808B along the major axis constructed using the data of emission lines H$\alpha$ and \[N II\] is shown in Fig.3b according to RC. It is seen that the galaxy demonstrates very peculiar kinematics: the kinematic center of the galaxy is shifted from the photomteric one by approximately 0.7" (0.3 kpc) to NE; after reaching the maximum value ($\rm V_{max}\,=\,120\pm10$ km/s) at $\rm r\approx3"$ the radial velocities show rapid decrease to the value nearly equal to the systematic velocity. According to classification of rotation curves for interacting galaxies suggested by Keel (1993) (Fig.2 in that paper) the rotation curve of NGC 3808B belongs to the group DIST (disturbed).

In Fig.6 the solid line represents the rotation curve of the galaxy averaged relative to the center and polinomially smoothed. Evidently it cannot reflect a real mass distribution in the galaxy but is a result of combined influence of gravitational disturbance from massive companion (NGC 3808A) and matter accretion from that to NGC 