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. the Low Frequency Array, LOFAR). Two different scenarios, in which the end of reionization occurs early (z ≈ 13) or late (z ≈ 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 H I 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 H I structures on arcmin scales, emitting at a brightness temperature of ≈35 mK as a 3σ signal in about 1000 h 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. © 2006 The Authors. Journal compilation © 2006 RAS.

Item Type:	Refereed Article
Research Division:	Physical Sciences
Research Group:	Astronomical sciences
Research Field:	Galactic astronomy
Objective Division:	Expanding Knowledge
Objective Group:	Expanding knowledge
Objective Field:	Expanding knowledge in the physical sciences
UTAS Author:	Johnston-Hollitt, M (Dr Melanie Johnston-Hollitt)
ID Code:	40454
Year Published:	2006
Web of Science® Times Cited:	10
Deposited By:	Physics
Deposited On:	2006-08-01
Last Modified:	2007-03-21
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