Fig. C.2.
In both panels, x-axis shows the input fluxes to model H II regions in a mock galaxy with an underlying diffuse component and y-axis shows the fluxes in H II regions after diffuse background subtraction. In both panels, the dashed red line is the one-to-one line. H II regions are modelled as the Moffat profiles with β = 1.5 (upper panel) and β = 2.5 (lower panel).
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