Angular power spectrum of brightness fluctuations in the ﹩\zeta =40﹩ model. The thick curves are for ﹩\overline{x}_{\mathrm{H}\,}=0.96﹩ (dotted), ﹩\overline{x}_{\mathrm{H}\,}=0.8﹩ (short‐dashed), ﹩\overline{x}_{\mathrm{H}\,}=0.5﹩ (long‐dashed), and ﹩\overline{x}_{\mathrm{H}\,}=0.26﹩ (solid). The thin long‐dashed curve is for the model where galaxies host their own individual H II regions (﹩\overline{x}_{\mathrm{H}\,}=0.5﹩).