Fig 3 - uploaded by F. Aharonian
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The spectral energy distribution of upscattered photons (in arbitrary units) for different values of the parameter b: b → 0, b = 5, 10, 30, and b → ∞ .
Source publication
In this paper we study the formation of giant electrons-positron pair halos around the powerful high energy extragalactic sources. We investigate the dependence of radiation of pair halos, in particular the spectral and angular distributions on the energy spectrum of the primary gamma-rays, the redshift of the source, and the flux of the extragalac...
Contexts in source publication
Context 1
... spectra of upscattered photons depend only on the parameter b, as illustrated in Fig. 3. If the value of b is small, as in the Thomson regime, the upscattered photon population is predominantly in the low energy regime. If the value of b is large, corresponding to the Klein-Nishina regime, the population is shifted towards high ...
Context 2
... including the formation and evolution of galaxies are included in the code. The EBL model M98 is based on empirical assumptions. It adopts an EBL flux at the present epoch (z = 0, and assumes time evolution proportional to (1 + z) 3.1 . These two EBL models for z = 0.129, as well as the corresponding mean free paths of gamma-rays are shown in Fig. 13 ...
Context 3
... Fig. 14 we show the SEDs and angular distributions of a pair halo located at z = 0.129 calculated for two EBL models shown in Fig. 13. One can see that while the SEDs are quite similar at low energies, the energy spectrum corresponding to the P00 model is significantly shifted compared to the SED predicted by the M98 EBL model. Also, the P00 EBL model predicts sharper angular distribution, especially at anant Very High Energy γ-rays from e ± Pair Halos 13 ≥ 0.1 • . ...
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