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Galactic winds are associated with intense star formation and AGNs. Dependingon their formation mechanism and velocity they may remove a significantfraction of gas from their host galaxies, thus suppressing star formation,enriching the intergalactic medium, and shaping the circumgalactic gas.However, the long-term evolution of these winds remains mostly unknown. Wereport the detection of a wind from NGC 3079 to at least 60 kpc from thegalaxy. We detect the wind in FUV line emission to 60 kpc (as inferred from thebroad FUV filter in GALEX) and in X-rays to at least 30~kpc. The morphology,luminosities, temperatures, and densities indicate that the emission comes fromshocked material, and the O/Fe ratio implies that the X-ray emitting gas isenriched by Type II supernovae. If so, the speed inferred from simple shockmodels is about 500 km/s, which is sufficient to escape the galaxy. However,the inferred kinetic energy in the wind from visible components issubstantially smaller than canonical hot superwind models.

A 60-kpc Galactic Wind Cone in NGC 3079