Same as Fig. 4, but 10% of the clouds orbits are visible. From left to right: columns show orbital segments (kT_cij/10, (k + 1)T_cij/10) for k ∈ {0, 4, 9} defined by the orbital period T_cij of the clouds. From the top down, panels a–c: elliptical binary system in which the orbital plane of the more massive SMBH is inclined by 30°, e = 0.5, Ω₁ = Ω₂ = 0°, ω₁ = 0, and ω₂ = 180°, and both discs are circular; panels d–f: same orbital configuration of the binary system as panels a–c, but their disc-like BLRs parameters are e_c1 = e_c2 = 0.5, Ω_c1 = Ω_c2 = 100°,ω_c1 = 110°, and ω_c2 = 290°; and panels g–i: same configuration of the binary system as panels a–c, and the orbital configurations of the BLR clouds are the same as in panels d–f, except that their eccentricities are random. The stability of the elliptical orbits in randomised motion is not considered.