Efficient simulation of discrete galaxy populations and associated radiation fields over the first billion years

Open Access

Fig. 9

21cm power spectra shown for the same five models as in Figure 8. We show the power-spectra at two points in cosmic history: the midway point of the EoR (the snapshot at which the total ionised fraction is closest to 50%), as well during X-ray heating where the volume-weighted mean brightness temperature $⟨ d T_{b, 21} ⟩$ $\langle dT_{b,21} \rangle$ is approximately zero.

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