...
In conclusion, the great window for high energy gamma-rays (10 GeV < E < 100 GeV) that GLAST will open will also provide unique insight into the optical-UV universe. Potentially, this will lay a path for a deeper understanding of the universe for many years to come.
[1] Kashlinsky review, A. 2005, PhR, 409, 361
[2] Hauser, M., & Dwek, E. 2001, ARA&A, 39, 249
[3] Stecker, F. W., de Jager, O. C., & Salamon, M. H. 1992, ApJL, 390, 49
[4] Dermer C. D. , 2006, ApJ, submitted (astro-ph/0605402)
[5] Chiang, J., & Mukherjee, R. 1998, ApJ, 496, 752
[6] Stecker, F. W., & Salamon, M. H. 1996, ApJ, 464, 600
[7] Narumoto & TotaniT., and Totani, T., 2006, ApJ, 643, 81
[8] Chen, A., Reyes, L. C. & Ritz, S. M. 2004, ApJ, 608, 686
[9] Kneiske, T., et al. 2004, A&A, 413, 807
[10] Fazio, G. G., & Stecker, F. W. 1970, Nature, 226, 135
[11] Anita's paperReimer, A. 2007, ApJ, submitted (astro-ph/0705.1534)
[12] Komin, N., Piron, F., & Pelassa, V. 2007, in Proc. of the 1st GLAST Symposium[12] Nukri and Fred
*************************************************************************************************************
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.
...