3808B on the gaseous disk of the latter. Let us find what rotation curve NGC 3808B would have if it was not a member of interacting pair. To do this we have approximated the inner part ($\rm r\leq2.5"$) of the observed rotation curve by the model of exponential disk (Monnet & Simien 1977) with intrinsic axial ratio $b/a\,=\rm\,0.2$ and the value of scale-length $h\,=\rm\,3.9"$ found earlier. The resulting curve depending besides $b/a$ on the only free parameter (mass-to-light ratio which is $f_{V}\,=\,$3.6 in solar units) is shown in Fig.6 by dashed line. This curve is hypothetical “non-disturbed” rotation curve of the galaxy. The maximum velocity of the model rotation curve is equal to 173 km/s at $\rm r=9"$ (4.1 kpc). Let us consider how it agrees with other global characteristics of the galaxy.

As it follows from integral colour indexes and surface brightness distribution, NGC 3808B belongs to Sc-Scd galaxies. Using the data on 207 spiral galaxies compiled by Corradi & Capaccipli (1991), Reshetnikov (1994) found the following dependence between numerical Hubble stage index ($T$) and maximum rotation velocity: $\rm V_{max}\,(km/s)\,=\,292\,-\,22.7$$T$. From this equation the value $\rm V_{max}\,\approx\,156-179$ km/s should be expected for NGC 3808B. The value of $\rm V_{max}$ 