Probing intergalactic radiation fields during cosmic reionization through gamma-ray absorption

TL;DR

This paper explores how high-energy gamma-ray absorption by intergalactic radiation fields at high redshifts can serve as a probe for cosmic reionization, using models consistent with various observational constraints.

Contribution

It introduces a semi-analytical model of intergalactic radiation fields including Population II and III stars, predicting gamma-ray attenuation during reionization.

Findings

UV IRF causes significant gamma-ray attenuation above 12 GeV at z~5

Attenuation extends down to 6-8 GeV at z>8-10

Potential observability with Fermi and next-gen gamma-ray telescopes

Abstract

We discuss expectations for the absorption of high-energy gamma-rays by gamma-gamma pair production with intergalactic radiation fields (IRFs) at very high redshifts (z~5-20), and the prospects thereof for probing the cosmic reionization era. For the evolving IRF, a semi-analytical model incorporating both Population II and Population III stars is employed, which is consistent with a wide variety of existing high-z observations including QSO spectral measurements, WMAP Thomson depth constraints, near-IR source count limits, etc. We find that the UV IRF below the Lyman edge energy with intensities in the range of a few times 10^{-19} erg cm^{-2} s^{-1} Hz^{-1} sr^{-1} can cause appreciable attenuation above ~12 GeV at z~5, down to ~6-8 GeV at z>~8-10. This may be observable in the spectra of blazars or gamma-ray bursts by the Fermi Gamma-ray Space Telescope or next generation facilities such as the Cherenkov Telescope Array, Advanced Gamma-ray Imaging System or 5@5, providing invaluable insight into early star formation and cosmic reionization.