  Galactic winds are associated with intense star formation and AGNs. Depending
on their formation mechanism and velocity they may remove a significant
fraction 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. We
report the detection of a wind from NGC 3079 to at least 60 kpc from the
galaxy. We detect the wind in FUV line emission to 60 kpc (as inferred from the
broad FUV filter in GALEX) and in X-rays to at least 30~kpc. The morphology,
luminosities, temperatures, and densities indicate that the emission comes from
shocked material, and the O/Fe ratio implies that the X-ray emitting gas is
enriched by Type II supernovae. If so, the speed inferred from simple shock
models is about 500 km/s, which is sufficient to escape the galaxy. However,
the inferred kinetic energy in the wind from visible components is
substantially smaller than canonical hot superwind models.
