Observational implications of heavy mass loss by the SS 433 system are considered. The gas flowing out through the outer Lagrangian point forms a disklike envelope (extended disk) which is illuminated by the precessing accretion disk of SS 433. The extended disk has the shape of a double cone, whose surface brightness at about 1 arcsec scale is sufficient for the disk to be detected by the Hubble Space Telescope and probably by a ground-based telescope. At a distance r is less than 0.15 arcsec from SS 433, one might expect to find a spirallike structure in the extended disk, which could be variable in the course of precession. Some evidence for outflowing gas streams near the system is discussed.