Discrepancy of masses in double galaxies

The estimations of integral masses of double galaxies are obtained taking as a basis recent observational data on 150 pairs of galaxies with measured radial velocities for both components. It is shown that the mean orbital mass‐to‐luminosity ratio essentially depends on a morphological type of double galaxies and on a kind of interaction between pair components. Minimal values of mass‐to‐luminosity ratio take place for double galaxies having linear features of interaction, namely: bridges, tails; as well for pairs with compact and Markarian components, too. The empirical relation between mass‐to‐luminosity ratio and linear separation of pair components do not indicate on an existence of a hidden stellar coronae around double galaxies.