Limits on the extragalactic background light in the Fermi era

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Fig. 6

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Upper limits solely due to the IntVHELumi criterion for different values of the bulk Lorentz factor Γ_L and the Doppler factor δ_D of the emitting region. With increasing Lorentz and Doppler factor, respectively, the limits become worse (see Eqs. (10) and (14)).

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