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HI Signal from Reionization Epoch | | Shiv K. Sethi
; | | Date: |
6 Aug 2005 | | Journal: | Mon.Not.Roy.Astron.Soc. 363 (2005) 818-830 | | Subject: | astro-ph | | Abstract: | We investigate the all-sky signal in redshifted atomic hydrogen (HI) line from the reionization epoch. HI can be observed in both emission and absorption depending on the ratio of Lyman-$alpha$ to ionizing flux and the spectrum of the radiation in soft xray. We also compute the signal from pre-reionization epoch and show that within the uncertainty in cosmological parameters, it is fairly robust. The main features of HI signal can be summarized as: (a) The pre-ionized HI can be seen in absorption for $
u simeq 10hbox{--}40
m MHz$; the maximum signal strength is $simeq 70hbox{--}100
m mK$. (b) A sharp absorption feature of width $la 5
m MHz$ might be observed in the frequency range $simeq 50 hbox{--}100
m MHz$, depending on the reionization history. The strength of the signal is proportional to the ratio of the Lyman-$alpha$ and the hydrogen-ionizing flux and the spectral index of the radiation field in soft xray (c) At larger frequencies, HI is seen in emission with peak frequency between $60hbox{--}100
m MHz$, depending on the ionization history of the universe; the peak strength of this signal is $simeq 50
m mK$. From Fisher matrix analysis, we compute the precision with which the parameters of the model can be estimated from a future experiment: (a) the pre-reionization signal can constrain a region in the $Omega_b h^2$--$Omega_m h^2$ plane (b) HI observed in emission can be used to give precise, $la 1 %$, measurement of the evolution of the ionization fraction in the universe, and (c) the transition region from absorption to emission can be used as a probe of the spectrum of ionizing sources; in particular, the HI signal in this regime can give reasonably precise measurement of the fraction of the universe heated by soft x-ray photons. | | Source: | arXiv, astro-ph/0508172 | | Services: | Forum | Review | PDF | Favorites | |
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