Individual spectra and atmospheric structure of selected clusters from the ch0l2023 simulation. From left to right, the first two columns show the Stokes I and V (normalized to the nearby continuum, around λ₀ + 0.95 nm), while the last three columns show the temperature, vertical velocity, and vertical magnetic field as a function of log τ₅₀₀₀. Each row depicts a different cluster. From the top, the first and second are #80 and #84 (from the numbering in Fig. 4), and represent some of the wider line profiles. The third and fourth rows depict cluster numbers #57 and #75, which represent some of the narrowest line profiles.