Semi-schematic visualization of the kinematic model. Left-hand panel: Column density map, N(x). Here, x denotes the on-sky position. The map was created by superposing four clouds with $N(\mathrm{C}\mathrm{I}\mathrm{V})={10}^{14}$ cm⁻² (cores) and 10¹² cm⁻² (halos) at random positions and line-of-sight velocities, v_c. The clouds are colored according to v_c. The white dot represents a narrow beam (e.g., a quasar pencil beam), and the four squares indicate wide beams (e.g., ARCTOMO spaxels). An optical-depth cube τ(v, x) was created by evaluating Voigt profiles (Liang & Kravtsov 2017) with v = v_c, N = N(x), and b = 10 km s⁻¹, and spectra were generated by averaging e^−τ within the beam area. Upper right panels: Wide-beam spectra at infinite and MUSE spectral resolution (HR and LR, respectively). The green squared symbols with error bars indicate LR individual line velocity centroids and σ_∥ dispersions, respectively, obtained from Gaussian fits. The shaded region indicates the overall σ_⊥ dispersion of the four LR velocities. Lower right panel: Narrow-beam spectrum at infinite spectral resolution. We note that v_c is indicated with the same colors as in the left-hand panel.