Study of Galaxy Evolution using VHE γ-ray Observations with Ground-based Cerenkov Telescopes

Details Study of Galaxy Evolution using VHE γ-ray Observations with Ground-based Cerenkov Telescopes Study of Galaxy Evolution using VHE γ-ray Observations with Ground-based Cerenkov Telescopes

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..204..151k&link_type=abstract

The Extragalactic Infrared Background and its Cosmological Implications, Proceedings of IAU Symposium #204, held 15-18 August 20

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The distribution of extra-galactic light (EBL) in the infrared (IR) spectral region wields important information on the evolution of galaxies. The spectrum of a galaxy in the 0.1-200μm range is a footprint of the starlight itself at ~1μm and extinction/emission of starlight by dust at ~ 100μm. The resulting spectral energy distribution (SED) of the EBL relies finally on galaxy luminosity evolution. The high energy γ-rays are absorbed by the EBL photons: γγ->e+e-. Such an effect has been seen recently in the Mkn 501 TeV spectrum measured by the HEGRA (High Energy Gamma Ray Astronomy) collaboration using the advanced system of imaging atmospheric Cerenkov telescopes (IACTs). The intrinsic spectra of AGNs in the 50 GeV-1 TeV energy range may be constrained by the X-ray fluxes measured with satellite instruments (RXTE, XMM, ASCA). Therefore by reducing the energy threshold down to 50 GeV forthcoming ground-based IACTs systems (CANGAROO IV, H. E. S. S., VERITAS) may be able to study the absorption cutoff in the energy spectra of distant AGNs (z<0.4), and to unfold the true galaxy luminosity evolution function.

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