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We study the statistical properties of the cosmological 21‐cm signal from both the intergalactic medium (IGM) and minihaloes, using a reionization simulation that includes a self‐consistent treatment of minihalo photoevaporation. We consider two models for minihalo formation and three typical thermal states of the IGM – heating purely by ionization, heating from both ionizing and Lyα photons and a maximal ‘strong heating’ model. We find that the signal from the IGM is almost always dominant over that from minihaloes. In our calculation, the differential brightness temperature,  δ T  b ,  of minihaloes is never larger than 2 mK. Although there are indeed some differences in the signals from the minihaloes and from the IGM, even with the planned generation of radio telescopes it will be unfeasible to detect them. However, minihaloes significantly affect the ionization state of the IGM and the corresponding 21‐cm flux.

The contribution of the IGM and minihaloes to the 21‐cm signal of reionization