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Super-massive black holes (SMBHs) spend most of their lifetime accreting at arate well below the Eddington limit, manifesting themselves as low-luminosityactive galactic nuclei (LLAGNs). The prevalence of a hot wind from LLAGNs is ageneric prediction by theories and numerical simulations of black holeaccretion and is recently becoming a crucial ingredient of AGN kinetic feedbackin cosmological simulations of galaxy evolution. However, direct observationalevidence for this hot wind is still scarce. In this work, we identifysignificant Fe XXVI Ly$\alpha$ and Fe XXV K$\alpha$ emission lines fromhigh-resolution Chandra grating spectra of the LLAGN in NGC\,7213, a nearby Sagalaxy hosting a $\sim10^8\rm~M_\odot$ SMBH, confirming previous work. We findthat these lines exhibit a blueshifted line-of-sight velocity of$\sim1100\rm~km s^{-1}$ and a high XXVI Ly$\alpha$ to XXV K$\alpha$ flux ratioimplying for a $\sim16$ keV hot plasma. By confronting these spectral featureswith synthetic X-ray spectra based on our custom magnetohydrodynamicalsimulations, we find that the high-velocity, hot plasma is naturally explainedby the putative hot wind driven by the hot accretion flow powering this LLAGN.Alternative plausible origins of this hot plasma, including stellar activities,AGN photoionization and the hot accretion flow itself, are quantitativelydisfavored. The inferred kinetic energy and momentum carried by the wind canserve as strong feedback to the environment. We compare NGC\,7213 to M81*, inwhich strong evidence for a hot wind was recently presented, and discussimplications on the universality and detectability of hot winds from LLAGNs.

Evidence for A Hot Wind from High-resolution X-ray Spectroscopic Observation of the Low-luminosity Active Galactic Nucleus in NGC 7213