Edge-on and face-on emission measure maps for the different simulated clumping scenarios (see text). In each case we assumed a mean hydrogen number density of n_H (h) = 0.1 cm⁻³ × e^{−|h|∕h₀}, where |h| is the distance from the galactic plane and h₀ = 1 kpc is the scale height of the gas. The simulations also share the same distribution and luminosities of the ionizing sources. The edge lengths of the maps are 5 kpc. The macroclumping case with f_cl = 5 appears generally very similar to the microclumping case with the same clumping factor, as is expected for sufficiently fine grid resolution. For f_cl = 25, the macroclumping becomes very porous at the used grid resolution, opening up channels devoid of gas that allow radiation to escape from the immediate environment of the sources without being absorbed. The combined micro- and macroclumping case with f_cl = 5 × 5 is very different from the macroclumping case with f_cl = 25, giving an overall appearance resembling that of the cases with f_cl = 5, but with theemission in each of the ionized bubbles more concentrated; this is somewhat analogous again to the transition from f_cl = 1 to f_cl = 5.