Scheme of the proposed scenario (not to scale). The wind ejected from the accretion disk of the SMBH interacts with the BHs forming the cluster. Because of the combination of the velocities of the SMBH wind (v_w) and the orbital motion of the BH (v_BH), a bow shock forms in the direction of the relative velocity (v_rel). The dense wind is captured by the BH via cylindrical accretion. A small accretion disk forms around the BH and jets are produced with two assumed shock-prone zones (recollimation and terminal regions).