Fig. 5
Left panel: SEDs from the population synthesis model, filtered as the stellar atmosphere models in Fig. 1. For our 3D simulations we use the SED of the model with fesc = 10% (magenta) as ionizing flux for the DIG. Right panel: corresponding energy-dependent escape fractions, as in Fig. 2. A comparison with Figs. 1 and 2 shows that the SEDs roughly resemble those using a 40 kK star.
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