Distributions of optical depth (upper row) and surface brightness (10 μm; lower row) for spectral types F4, G4, K4, and M4, from left to right, assuming a constant τ_BG ∼ 3 zodis. The star is located at the center of the distributions, and the planet is marked with a white dot to the right of the central star. The spatial scale differs between the upper and lower panels: the optical depth maps show a larger region (∼4 a_p) to capture the full disk structure, while the surface brightness provides a zoom-in on a smaller region (∼2 a_p) around the planet to emphasize resonant ring structures. All panels have a consistent bin size of a_p/50 × a_p/50. The color bars vary across spectral types to optimize visualization. For reference, the optical depth at r ∼ 2 a_p is τ_BG ≈ 2.1 × 10⁻⁷ for all spectral types. The inner regions of the surface brightness maps are saturated above the ring maximum and excluded within the sublimation distance. The spatial scale also varies with spectral type, with lower-mass stars having more compact configurations. These results correspond to Model II only, as they are from the main study. Note that we derive our results from grain sizes of 0.1-300 μm and may differ if larger grains are included (see Sect. 4.5).