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Radio views of cosmic reionization

Version 2 2024-09-17, 02:12
Version 1 2023-05-16, 18:08
journal contribution
posted on 2024-09-17, 02:12 authored by M Valdes, B Ciardi, A Ferrara, M Johnston-Hollitt, H Rottgering
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.

History

Publication title

Monthly Notices of the Royal Astronomical Society

Volume

369

Issue

1

Pagination

L66-L70

ISSN

0035-8711

Department/School

School of Natural Sciences

Publisher

Blackwell Publishing

Publication status

  • Published

Place of publication

London, England

Socio-economic Objectives

280120 Expanding knowledge in the physical sciences

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