This paper presents a study of millimeter-wave images of geometrically thick accretion disks and funnel walls around Kerr black holes, using an analytical model of magnetofluids. The model, based on the horizon-scale magnetofluid model developed in [1], investigates the optical appearances of these structures by solving the null geodesic and radiative transfer equations. The study focuses on the thermal synchrotron radiation emitted by the magnetofluid, which is the primary source of light in black hole imaging. For the thick disk, the impact of emission anisotropy on images is examined, showing that anisotropic synchrotron radiation plays a significant role in the observability of the photon ring. For the funnel wall, both outflow and inflow models are considered, with the outflow funnel wall producing a brighter primary image than the photon ring, while the inflow funnel wall does not. The inflow funnel wall model is not ruled out by current observations of M87*. The study also explores the images of black holes illuminated by the funnel wall, considering both outward and inward flows. The outflow model produces excessively bright primary images of jet bases, potentially leading to the absence of the black hole shadow, which is inconsistent with current observations of M87*. In contrast, the inflow funnel wall model is consistent with observations. The results show that the brightness of the primary image of the jet base is significantly diminished compared to the photon ring due to the inward flow. The study also investigates the effect of absorption on the observed intensity, finding that lower frequencies are more affected by absorption, while higher frequencies are less affected. The findings are consistent with the inflow dual cone model presented in [64]. The study concludes that the analytical model provides a valid description of the morphology of thick disks and funnel walls at the horizon scale, although it has certain limitations, such as the assumption of a radial magnetic field and the simplification of the fluid dynamics. The results are in agreement with current observations and provide insights into the structure and behavior of black hole environments.This paper presents a study of millimeter-wave images of geometrically thick accretion disks and funnel walls around Kerr black holes, using an analytical model of magnetofluids. The model, based on the horizon-scale magnetofluid model developed in [1], investigates the optical appearances of these structures by solving the null geodesic and radiative transfer equations. The study focuses on the thermal synchrotron radiation emitted by the magnetofluid, which is the primary source of light in black hole imaging. For the thick disk, the impact of emission anisotropy on images is examined, showing that anisotropic synchrotron radiation plays a significant role in the observability of the photon ring. For the funnel wall, both outflow and inflow models are considered, with the outflow funnel wall producing a brighter primary image than the photon ring, while the inflow funnel wall does not. The inflow funnel wall model is not ruled out by current observations of M87*. The study also explores the images of black holes illuminated by the funnel wall, considering both outward and inward flows. The outflow model produces excessively bright primary images of jet bases, potentially leading to the absence of the black hole shadow, which is inconsistent with current observations of M87*. In contrast, the inflow funnel wall model is consistent with observations. The results show that the brightness of the primary image of the jet base is significantly diminished compared to the photon ring due to the inward flow. The study also investigates the effect of absorption on the observed intensity, finding that lower frequencies are more affected by absorption, while higher frequencies are less affected. The findings are consistent with the inflow dual cone model presented in [64]. The study concludes that the analytical model provides a valid description of the morphology of thick disks and funnel walls at the horizon scale, although it has certain limitations, such as the assumption of a radial magnetic field and the simplification of the fluid dynamics. The results are in agreement with current observations and provide insights into the structure and behavior of black hole environments.