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The ionisation structure of the Intergalactic Medium (IGM) duringreionisation is sensitive to the unknown galaxy formation physics thatprevailed at that time. This structure introduces non-Gaussian statistics intothe redshifted 21 cm fluctuation amplitudes that can only be studied throughtomographic imaging, which will clearly discriminate between different galaxyformation scenarios. Imaging the ionisation structure and cosmological HIIregions during reionisation is therefore a key goal for the SKA. For example,the SKA1-LOW baseline design with a 1 km diameter core will resolve HII regionsexpected from galaxy formation models which include strong feedback on low-massgalaxy formation. Imaging the smaller HII regions that result from galaxyformation in the absence of SNe feedback will also be possible for SKA1-LOW inthe later stages of reionisation, but may require the greater sensitivity ofSKA early in the reionisation era. In addition to having baselines long enoughto resolve the HII regions, the field of view for SKA1-LOW reionisationexperiments should be at least several degrees in order to image the largest HIstructures towards the end of reionisation. The baseline design with 35 meterdiameter stations has a field of view within a single primary pointing which issufficient for this purpose.

Imaging HII Regions from Galaxies and Quasars During Reionisation with SKA