The Extragalactic Background at Ultraviolet X-ray, and Gamma-ray Energies

Details The Extragalactic Background at Ultraviolet X-ray, and Gamma-ray Energies The Extragalactic Background at Ultraviolet X-ray, and Gamma-ray Energies

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..204..123b&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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Initial work on these backgrounds was motivated, at least in part, by the idea that these fluxes were the result of some truly diffuse source with possibly profound cosmological implications. Ongoing research shows that these backgrounds are the summed product of individual sources, but in some cases the sources themselves have not been identified. The extragalactic UV background is exceedingly difficult to measure because of competing backgrounds and individual sources in our own galaxy. It is uncertain whether an extragalactic component has been measured, much less characterized. Sixty to ninety percent of the 0.5 to 2 KeV X-ray background has been identified with AGN and clusters of galaxies. Roughly half of the 2 to 6 KeV background can be attributed to AGN's but the remaining flux must be produced by sources which are currently unidentified. These sources must undergo both spectral and clustering evolution since extrapolations of ``nearby'' sources cannot produce the required flux. The background from 300 KeV to 10 MeV is conjectured to be the summed result of extragalactic supernovae. The flux above these energies emanates from discrete sources, thought to be blazars, rather than a diffuse background.

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