  Based on the horizon-scale magnetofluid model developed in
[arXiv:2309.13304], we investigate the millimeter-wave images of a
geometrically thick accretion disk or a funnel wall, i.e., the magnetofluid
that encloses the base of the jet region, around a Kerr black hole. By
employing the numerical method to solve the null geodesic and radiative
transfer equations, we obtain the optical appearances at various observational
angles and frequencies, generated by the thermal synchrotron radiation within
the magnetofluid. For the thick disk, we specifically examine the impact of
emission anisotropy on images, concluding that anisotropic synchrotron
radiation could play an important role in the observability of the photon ring.
For the funnel wall, we find that both the outflow and inflow funnel walls
exhibit annular structures on the imaging plane. The outflow funnel wall yields
a brighter primary image than the photon ring, whereas the inflow one does not.
Based on our investigation, the inflow funnel wall model can not be ruled out
by current observations of M87*.
