r\approx\pm30"$ from the nucleus the surface brightness decreases very slowly, then falls down more rapidly. Note that the profile shows no signs of pronounced bulge in the central region of the galaxy (partly may be due to absorption of the bulge emission by dust lane projected onto the central region - see Fig.8,9). The equivalent luminosity profile of the galaxy is shown in Fig.11. As one can see, up to $\rm r^{*}\approx20"$ (or $\mu(B)\approx$24) the averaged surface brightness distribution of the galaxy is well described by exponential law with parameters $\mu_{0}(B)\rm=20.37$, $h^{*}=$6.6" (dashed line in Fig.11), then the profile changes its slope and becomes more flat (see also the equivalent profile in the $R$ passband published in Reshetnikov et al. (1993a)). This change at $\rm r^{*}\approx20"$ is probably due to the contribution of ring-like structure surrounding the galaxy. Let us note also that the central surface brightness of the galactic disk is considerably brighter than canonical value $\mu_{0}(B)=$21.65 (Freeman 1970). Such a property is typical for the galaxies in interacting systems (Reshetnikov et al. 1993b).

The distribution of $z_{0}$ values along the disk of NGC 6286 is shown in Fig.12 for three passbands. To exclude the influence of ring-like structure 