For most of their lifetime, super-massive black holes (SMBHs) commonly found in galactic nuclei obtain mass from the ambient at a rate well below the Eddington limit, which is mediated by a radiatively inefficient, hot accretion flow. Both theory and numerical simulations predict that a strong wind must exist in such hot accretion flows. The wind is of special interest not only because it is an indispensable ingredient of accretion, but perhaps more importantly, it is believed to play a crucial role in the evolution of the host galaxy via the so-called kinetic mode AGN feedback. Observational evidence for this wind, however, remains scarce and indirect. Here we report the detection of a hot outflow from the low-luminosity active galactic nucleus in M81, based on {it Chandra} high-resolution X-ray spectroscopy. The outflow is evidenced by a pair of Fe XXVI Ly$alpha$ lines redshifted and blueshifted at a bulk line-of-sight velocity of $pm2.8times10^3 rm~km~s^{-1}$ and a high Fe XXVI Ly$alpha$-to-Fe XXV K$alpha$ line ratio implying a plasma temperature of $1.3times10^8$ Kelvin. This high-velocity, hot plasma cannot be produced by stellar activity or the accretion inflow onto the SMBH. Our magnetohydrodynamical simulations show, instead, it is naturally explained by a wind from the hot accretion flow, propagating out to $gtrsim10^6$ times the gravitational radius of the SMBH. The kinetic energy and momentum of this wind can significantly affect the evolution of the circumnuclear environment and beyond.
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