We analyze the structure of the cluster of galaxies Abell 1775 ( \alpha = 13 ^ { h } 42 ^ { m } , \delta = +26 \degr 22 ^ { \prime } , cz \approx 21000 Â km/s ) , which exhibits a bimodal distribution of radial velocities of the containing galaxies . The difference of the subcluster radial velocities is \Delta V \approx 2900 Â km/s . We use the results of our photometric observations made with the 1-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and the spectroscopic and photometric data from the SDSS DR6 catalog to determine independent distances to the subclusters via three different methods : the Kormendy relation , photometric plane , and fundamental plane . We find that the A1775 cluster consists of two independent clusters , A1775A ( cz = 19664 Â km/s ) and A1775B ( cz = 22576 Â km/s ) , each located at its own Hubble distance and having small peculiar velocities . Given the velocity dispersions of 324Â km/s and 581Â km/s and the dynamic masses within the R _ { 200 } radius equal to 0.6 \times 10 ^ { 14 } and 3.3 \times 10 ^ { 14 } M _ { \odot } , the A1775A and A1775B clusters have the K-band luminosity-to-mass ratios of 29 and 61 , respectively . A radio galaxy with an extended tail belongs to the A1775B cluster .