  Jets are endemic to both Galactic solar mass and extragalactic supermassive
black holes. A recent 86 GHz image of M\,87 shows a jet emerging from the
accretion ring around a black hole, providing the first direct observational
constraint on the kinematics of the jet-launching region in any black hole
jetted system. The very wide ($\sim280\mu\rm{as}$), highly collimated,
limb-brightened cylindrical jet base is not predicted in current numerical
simulations. The emission was shown to be consistent with that of a
thick-walled cylindrical source that apparently feeds the flow that produces
the bright limbs of the outer jet at an axial distance downstream of $0.4
\,\rm{mas}<z<0.65\, \rm{mas}$. The analysis here applies the conservation laws
of energy, angular momentum, and magnetic flux to the combined system of the
outer jet, the cylindrical jet, and the launch region. It also uses the
brightness asymmetries of the jet and counterjet to constrain the Doppler
factor. The only global solutions have a source that is located $<34
\mu\rm{as}$ from the event horizon. This includes the Event Horizon Telescope
annulus of emission and the regions interior to this annulus. The axial jet
begins as a magnetically dominated flow that spreads laterally from the launch
radius ($<34 \mu\rm{as}$). It becomes super-magnetosonic before it reaches the
base of the cylindrical jet. The flow is ostensibly redirected and collimated
by a cylindrical nozzle formed in a thick accretion disk. The flow emerges from
the nozzle as a mildly relativistic ($0.3c<v<0.4c$) jet with a significant
protonic kinetic energy flux.
