  Context. The tropospheric wind pattern in Jupiter consists of alternating
prograde and retrograde zonal jets with typical velocities of up to 100 m/s
around the equator. At much higher altitudes, in the ionosphere, strong auroral
jets have been discovered with velocities of 1-2 km/s. There is no such direct
measurement in the stratosphere of the planet. Aims. In this paper, we bridge
the altitude gap between these measurements by directly measuring the wind
speeds in Jupiter's stratosphere. Methods. We use the Atacama Large
Millimeter/submillimeter Array's very high spectral and angular resolution
imaging of the stratosphere of Jupiter to retrieve the wind speeds as a
function of latitude by fitting the Doppler shifts induced by the winds on the
spectral lines. Results. We detect for the first time equatorial zonal jets
that reside at 1 mbar, i.e. above the altitudes where Jupiter's
Quasi-Quadrennial Oscillation occurs. Most noticeably, we find 300-400 m/s
non-zonal winds at 0.1 mbar over the polar regions underneath the main auroral
ovals. They are in counter-rotation and lie several hundreds of kilometers
below the ionospheric auroral winds. We suspect them to be the lower tail of
the ionospheric auroral winds. Conclusions. We detect directly and for the
first time strong winds in Jupiter's stratosphere. They are zonal at low-to-mid
latitudes and non-zonal at polar latitudes. The wind system found at polar
latitudes may help increase the effciency of chemical complexification by
confining the photochemical products in a region of large energetic electron
precipitation.
