We use numerical simulations of cosmic reionization and radiative processes related to the HI 21 cm emission line to produce synthetic radio maps as seen by next generation telescopes that will operate at low radio frequencies ( e.g .
LOFAR ) .
Two different scenarios , in which the end of reionization occurs early ( z \approx 13 ) or late ( z \approx 8 ) depending on the Initial Mass Function ( IMF ) of the first stars and ionizing photon escape fraction , have been explored .
For each of these models we produce synthetic HI 21 cm emission maps by convolving the simulation outputs with the provisional LOFAR sampling function in the frequency range 76-140 MHz .
If reionization occurs late , LOFAR will be able to detect individual HI structures on arcmin scales , emitting at a brightness temperature of \approx 35 mK as a 3- \sigma signal in about 1000 hours of observing time .
In the case of early reionization , the detection would be unlikely , due to decreased sensitivity and increased sky temperatures .
These results assume that ionospheric , interference and foreground issues are fully under control .