  The polarized images of the supermassive black hole Messier 87* (M87*)
produced by the Event Horizon Telescope (EHT) provide a direct view of the
near-horizon emission from a black hole accretion and jet system. The EHT
theoretical analysis of the polarized M87* images compared thousands of
snapshots from numerical models with a variety of spins, magnetization states,
viewing inclinations, and electron energy distributions, and found a small
subset consistent with the observed image. In this article, we examine two
models favored by EHT analyses: a magnetically arrested disk with moderate
retrograde spin and a magnetically arrested disk with high prograde spin. Both
have electron distribution functions which lead to strong depolarization by
cold electrons. We ray trace five snapshots from each model at 22, 43, 86, 230,
345, and 690 GHz to forecast future VLBI observations and examine limitations
in numerical models. We find that even at low frequencies where optical and
Faraday rotation depths are large, approximately rotationally symmetric
polarization persists, suggesting that shallow depths dominate the polarization
signal. However, morphology and spectra suggest that the assumed thermal
electron distribution is not adequate to describe emission from the jet. We
find 86 GHz images show a ring-like shape determined by a combination of plasma
and spacetime imprints, smaller in diameter than recent results from the Global
mm-VLBI array. We find that the photon ring becomes more apparent with
increasing frequency, and is more apparent in the retrograde model, leading to
large differences between models in asymmetry and polarization structure.
