this case we deal with gravitationally bound galaxies interacting over a long time but not with chance encounter. In many aspects NGC 3808 resembles interacting system NGC 7753/52 (Arp 86) in which mass transfer occurs from main galaxy to low-massive companion (Laurikainen et al. 1993, Salo & Laurikainen 1993). As in NGC 3808B, the accretion of matter to NGC 7752 results in global bursts of star formation in this galaxy. Numerical modeling shows that the components of Arp 86 are moving in a low-eccentricity relative orbit. By analogy, we suggest that the members of NGC 3808 are also at nearly circular relative orbit favourable to mass transfer.

NGC 6286 (PRC C-51)
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NGC 6285/6 (Arp 293) is an interacting double system resembling NGC 3808A,B. The mean difference between them is that in the case of NGC 6285/6 both galaxies have comparable masses. For $\rm D\,=\,$76.5 Mpc (RC) the angular distance between galaxies (1.5’) corresponds to the projected distance of 33 kpc. The radial velocity difference is not well known but seems to be no more than 200 km/s (NED[^1]).

In Fig.8 the reproductions of $B$-band CCD image of NGC 6286 (just this galaxy is a candidate to PRG) are shown 