  Wind and jet are important medium of AGN feedback thus it is crucial to
obtain their properties for the feedback study. In this paper we investigate
the properties of wind and jet launched from a magnetized super-Eddington
accretion flow around a supermassive black hole. For this aim, we have
performed radiation magnetohydrodynamical simulation of a magnetically arrested
super-Eddington accretion flows. We then have analyzed the simulation data by
the ``virtual particle trajectory'' approach and obtained the mass flux,
poloidal and toroidal velocities, and mass-flux-weighted momentum and energy
fluxes of wind and jet. The mass flux is found to be 2-6 times higher than that
obtained based on the time-averaged streamline method widely used in
literature. The momentum flux of wind is found to be larger than that of jet,
while the total energy flux of jet is at most 3 times larger than that of wind.
These results are similar to the case of hot accretion flows and imply that
winds likely play a more important role than jet in AGN feedback. The
acceleration mechanism of wind and jet is analyzed and found to be dominated by
Lorentz force rather than radiation force.
