Line ratio maps from microclumped models (f_cl = 5) as in the leftmost columns of Figs. 7 and 8, using the same simulation volume and the same integrated hydrogen-ionizing flux as before, but taking the unfiltered spectrum of a 35 kK dwarf star with solar metallicity as the ionizing SED. The most notable difference to the models using the population SED is the weaker emission of the optical [O III] lines. The emission of the [N II] and [O II] lines is stronger close to the galactic plane, but shows a weaker rise close to the edge of the simulated volume.