Detection of a Far IR Excess with DIRBE at 60 and 100 Microns

Details Detection of a Far IR Excess with DIRBE at 60 and 100 Microns Detection of a Far IR Excess with DIRBE at 60 and 100 Microns

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..204..121f&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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From analysis of the DIRBE weekly averaged sky maps, we have detected substantial flux in the 60 micron and 100 micron channels in excess of expected zodiacal and Galactic emission (Finkbeiner et al. 2000, astro-ph/0004175). Two methods are used to separate zodiacal light from more distant emission. Both methods give consistent results at 60 micron and 100 micron. The observed signal is consistent with an isotropic background at the level ν Iν = 28.1 ± 1.8 ± 7(syst)nWpMMSr at 60 micron and 24.6 ± 2.5 ± 8nWpMMSr at 100 micron. The IR excess detected at 140 and 240 micron by these methods agrees with previous measurements, which are thought to be the cosmic infra-red background (CIB). The detections at 60 and 100 micron are new. While this new excess is not necessarily the CIB, we have ruled out all known sources of emission in the solar system and Galaxy. We therefore tentatively interpret this signal as the CIB and consider the implications of such energy production from the viewpoint of star formation efficiency and black hole accretion efficiency. However, the IR excess exceeds limits on the CIB derived from the inferred opacity of the IGM to observed TeV photons, thus casting doubt on this interpretation. There is currently no satisfactory explanation for the 60-100 micron excess.

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