Simulating the 21 cm forest detectable with LOFAR and SKA in the spectra of high-z GRBs

Journal
Date Issued
2015
Author(s)
Ciardi, B.
•
Inoue, S.
•
Abdalla, F. B.
•
Asad, K.
•
•
Bolton, J. S.
•
Brentjens, M.
•
de Bruyn, A. G.
•
Chapman, E.
•
Daiboo, S.
•
Fernandez, E. R.
•
Ghosh, A.
•
Graziani, L.
•
Harker, G. J. A.
•
Iliev, I. T.
•
Jelić, V.
•
Jensen, H.
•
Kazemi, S.
•
Koopmans, L. V. E.
•
Martinez, O.
•
Maselli, A.
•
Mellema, G.
•
Offringa, A. R.
•
Pandey, V. N.
•
Schaye, J.
•
Thomas, R.
•
Vedantham, H.
•
Yatawatta, S.
•
Zaroubi, S.
DOI
Description
The authors thank an anonymous referee for his/her useful comments. BC acknowledges Benoit Semelin for interesting discussions. This work was supported by DFG Priority Programs 1177 and 1573. SI appreciates support from Grant-in-Aid for Scientific Research No. 24340048 from MEXT of Japan. GH has received funding from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007–2013) under REA grant agreement no. 327999. LVEK, HV, KA and AG acknowledge the financial support from the European Research Council under ERC-Starting Grant FIRSTLIGHT - 258942. ITI was supported by the Science and Technology Facilities Council [grant number ST/L000652/1]. VJ would like to thank the Netherlands Foundation for Scientific Research (NWO) for financial support through VENI grant 639.041.336. JSB acknowledges the support of a Royal Society University Research Fellowship.
Abstract
We investigate the feasibility of detecting 21 cm absorption features in the afterglow spectra of high redshift long Gamma Ray Bursts (GRBs). This is done employing simulations of cosmic reionization, together with estimates of the GRB radio afterglow flux and the instrumental characteristics of the LOw Frequency ARray (LOFAR). We find that absorption features could be marginally (with a S/N larger than a few) detected by LOFAR at z ≳ 7 if the GRB is a highly energetic event originating from Pop III stars, while the detection would be easier if the noise were reduced by one order of magnitude, i.e. similar to what is expected for the first phase of the Square Kilometre Array (SKA1-low). On the other hand, more standard GRBs are too dim to be detected even with ten times the sensitivity of SKA1-low, and only in the most optimistic case can a S/N larger than a few be reached at z ≳ 9.
Volume
453
Issue
1
Start page
101
Uri
Url
Issn Identifier
0035-8711
Ads BibCode
2015MNRAS.453..101C
Rights
open.access
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