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We study Faraday rotation in the jet of M87 inside the Bondi radius usingeight Very Long Baseline Array data sets, one at 8 GHz, four at 5 GHz, andthree at 2 GHz. We obtain Faraday rotation measures (RMs) measured across thebandwidth of each data set. We find that the magnitude of RM systematicallydecreases with increasing distance from the black hole from 5,000 to 200,000Schwarzschild radii. The data, showing predominantly negative RM sign withoutsignificant difference of the RMs on the northern and southern jet edges,suggest that the spatial extent of the Faraday screen is much larger than thejet. We apply models of hot accretion flows, thought to be prevalent in activegalactic nuclei having relatively low luminosity such as M87, and find that thedecrease of RM is described well by a gas density profile $\rho \proptor^{-1}$. This behavior matches the theoretically expected signature ofsubstantial winds, nonrelativistic un-collimated gas outflows from hotaccretion flows, which is consistent with the results of various numericalsimulations. The pressure profile inferred from the density profile is flatenough to collimate the jet, which can result in gradual acceleration of thejet in a magneto-hydrodynamical process. This picture is in good agreement withthe observed gradual collimation and acceleration of the M87 jet inside theBondi radius. The dominance of negative RMs suggests that jet and wind axis aremisaligned such that the jet emission exposes only one side of the toroidalmagnetic fields permeating the winds.

Faraday rotation in the jet of M87 inside the Bondi radius: indication of winds from hot accretion flows confining the relativistic jet