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We present 3D hydrodynamical simulations of a precessing jet propagatinginside a supernova remnant (SNR) shell, particularly applied to the W50-SS433system in a search for the origin of its peculiar elongated morphology. Severalruns were carried out with different values for the mass loss rate of the jet,the initial radius of the SNR, and the opening angle of the precession cone. Wefound that our models successfully reproduce the scale and morphology of W50when the opening angle of the jets is set to 10$\degr$ or if this anglelinearly varies with time. For these models, more realistic runs were madeconsidering that the remnant is expanding into an interstellar medium (ISM)with an exponential density profile (as HI observations suggest). Taking intoaccount all these ingredients, the large scale morphology of the W50-SS 433system, including the asymmetry between the lobes (formed by the jet-SNRinteraction), is well reproduced.

Erratum: Three‐dimensional hydrodynamical simulations of the large‐scale structure of W50‐SS433