  Jet models of Event Horizon Telescope (EHT) data should also conform to the
observed jet profiles just downstream. This study evaluates conformance of
models of black hole jets to images of the innermost jet of M87. This is a
basic test that should be passed before using them to perform a physical
interpretation of EHT data. Recent 86 GHz Very Long Baseline Interferometry
observations of M87 have revealed the morphology and size of the jet near its
source ($<65$\,M, or 0.06 lt-yrs after correcting for line of sight to the jet,
where $M$ is the black hole mass in geometrized units) for the first time.
Current transverse resolution indicates that this region is dominated by flux
emanating from the edge of the jet. The observed inner jet profiles are
compared to all existing published synthetic radio images constructed from
"state of the art" 3-D numerical simulations of the black hole accretion system
in M87. Despite efforts to produce the characteristic wide, edge dominated jet,
these models are too narrow (by a factor of $\sim2$) in the region 0.06 - 0.32
lt-yrs from the source, even though the jets (spine and/or sheath) in the image
plane might appear conformant farther downstream. Furthermore, the synthetic
radio images are not edge dominated 0.06 - 0.32 lt-yrs from the source, but
spine dominated. Analyses that implement these models as physical diagnostics
of EHT visibility amplitudes are therefore suspect. Thus, these inner jet
characteristics are important considerations before applying simulations to the
EHT data.
