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We compared the molecular clouds in the western part of SS 433 withnear-ultraviolet radiation data obtained from GALEX. Near-ultraviolet radiationis prominently confirmed toward only N4, while no near-ultraviolet radiation isdetected toward N1, N2, and N3. The radiative region of near-ultravioletradiation is nearly the same as the CO-emitting region in N4, and does notextend beyond the jet seen in X-ray radiation. Near-ultraviolet radiationcannot be explained solely by broadband continuous radiation and may originatefrom line emissions. The intensity of near-ultraviolet radiation exhibits ananti-correlation with that of 13CO(J=3-2) emission. This anti-correlation,along with strong far-infrared radiation in the region with weakernear-ultraviolet radiation intensity compared to its surroundings, suggeststhat near-ultraviolet radiation originates from behind the molecular cloud,heating up the interstellar dust in N4. Subsequently, the dust in N4re-radiates in the far-infrared band. In the same region, a high peak T_MBratio of 12CO(J=3-2)/12CO(J=1-0) of ~0.9, and a high kinetic temperature of T_k~56 K in the molecular cloud indicate that CO molecules are highly excited, andthe molecular cloud is heated through photoelectric heating. This heatingresults from electrons released due to the photoelectric effect caused by thephenomenon where interstellar dust absorbs near-ultraviolet radiation. In termsof the timescale of near-ultraviolet radiation originating from line emissions,near-ultraviolet radiation towards N4 cannot be explained by the shock of theblast wave from a supernova that created W 50. These findings also suggest thatN4 directly interacts with the jet from SS 433. As a result of this directinteraction, near-ultraviolet radiation is emitted from an interacting layerbetween the jet and N4.

Near-Ultraviolet Radiation toward Molecular Cloud N4 in W 50/SS 433: Evidence for Direct Interaction of the Jet with Molecular Cloud