...
*************************************************************************************************************
Figure 1. Schematic EBL spectrum as a function of wavelength. The EBL spectrum consists of two spectral humps: The blue hump at UV-Optical-NIR wavelengths is the radiated output from stars. The red hump at MIR (mid-infrared) and FIR (far-infrared) wavelengths results from the absorption and re-emission of starlight by the interstellar medium. The CMB spectrum (dashed black line) is presented here just for comparison purposes (since it is not considered part of the EBL). The location and size of the humps is just approximate, since the precise shape and intensity of the EBL is not completely constrained from observations.
Figure 2. Fazio Stecker Relation for the simulated data. The black squares represent the energy cut-offs determined from the fits and their uncertainties. They converge to the EBL model (Kneiske et al. - best fit) used for the simulation (red line). Also shown is a different EBL model (Kneiske et al. - high-UV ; blue dashed line) used here to illustrate the discriminating power of the analysis.