SE part (semi-ring well seen in Fig.8b) has mean observed surface brightness $\mu(B)\approx$24 while its NW part is fainter by approximately $\rm 1^{m}$ (as NW part we imply the nearest to NGC 6286 region of the bridge connecting two galaxies). The total magnitude of forming ring in the $B$ band is $\rm 16.0\pm0.3$. Therefore, the contribution of the ring to the total luminosity of the galaxy is as high as 20%. Observed integral colour indexes of SE part of the ring ($B-V\,=\rm\,+0.56\pm0.06$, $V-R\,=\rm\,
+0.36\pm0.05$) are more blue than those of main galaxy. But after correction for inclination of the galaxy to the line of sight the colour indexes of both are very close. It should be noted also that colour index $B-V$ ($\rm\approx +0.8$) of the bridge between galaxies is somewhat redder than that of the main body of NGC 6286.

The distribution of radial velocities along the minor axis of NGC 6286 found from measurements of emission lines H$\alpha$ and \[NII\]$\lambda$6583 in RC (where NGC 6286 is named NGC 6285 by mistake) is shown in Fig.13b. One can suppose that there are two subsystems of gas in the galaxy. One of them well seen at $\rm r\approx$20" in H$\alpha$ 