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A high sensitivity, 7mm Very Long Baseline Array image of M\,87 waspreviously analyzed in order to estimate the bulk flow jet velocity between 0.4and 0.65 mas from the point of origin using the asymmetry between thewell-characterized double-ridged counter-jet (unique to this image) and thedouble ridged jet. We use this same image to estimate the cross-sectional areaof this tubular stream. The velocity, acceleration, cross-sectional area andflux density along this stream determines a unique, perfect magnetohydrodynamicjet solution that satisfies, conservation of energy, angular momentum and mass(a monotonic conversion of Poynting flux to kinetic energy flux along the jet).The solution is protonic and magnetically dominated. The bilateral jettransports $\approx 1.2\times10^{-4} M_{\odot}/\rm{yr}$ and $\approx1.1\times10^{42}$ erg/sec, placing strong constraints on the central engine. AKeplerian disk source that also produces the Event Horizon Telescope (EHT)annulus of emission can supply the energy and mass if the vertical magneticfield at the equator is $\sim 1-3.5$ G (depending on location). A Parker spiralmagnetic field, characteristic of a wind or jet, is consistent with theobserved EHT polarization pattern. Even though there is no image of the jetconnecting with the annulus, it is argued that these circumstances are notcoincidental and the polarized portion of the EHT emission is mainly jetemission in the top layers of the disk that is diluted by emission from anunderlying turbulent disk. This is a contributing factor to the relatively lowpolarization levels that were detected.

Did the Event Horizon Telescope Detect the Base of the Sub-Milliarsecond Tubular Jet in M\,87?