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

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.

MNRAS in press with minor revisions, 5 pages, 5 figures. Numerical data of the model results will be available at http://www-tap.scphys.kyoto-u.ac.jp/~inoue/hizabs/

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• Can Gamma-Ray Burst Jets Break Out the First Stars?
• Population III GRB Afterglows: Constraints on Stellar Masses and External Medium Densities
• Constraining the PopIII IMF with high-z GRBs
• Upper Bound on the First Star Formation History
• X-ray and Radio Follow-up Observations of High-Redshift Blazar Candidates in the Fermi-LAT Unassociated Source Population