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Limits on the Energy Density of the Cosmic Infrared Background

Published online by Cambridge University Press:  08 February 2017

Yoel Rephaeli  and
Reinhard Schlickeiser
Yoel Rephaeli
Affiliation:
School of Physics and Astronomy Tel Aviv University Tel Aviv, Israel
Reinhard Schlickeiser
Affiliation:
Max-Planck Institüt für Radioastronomie Bonn, FRG

Extract

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One of the least known regions of the cosmic electromagnetic background is in the infrared (IR). This infrared background (IRB) is of considerable astrophysical interest. Early stellar activity, either pregalactic (Bond, Carr and Hogan, 1986), or galactic (Partridge and Peebles, 1967), may have contributed significantly to the IRB. More significant, perhaps, are the superimposed IR emissions from normal galaxies, Seyferts, quasars, and rich clusters of galaxies (e.g., Stecker, Puget and Fazio, 1977). There are only few reported measurements of the IRB, which in general yield energy densities comparable to that of the Cosmic Microwave Background (CMB), ρo ≈4 10−13 erg cm−3. An upper limit on the energy density at 2 μm is δ ≡ ρ/ρo≤1.2 (Hoffman and Lemke, 1978). Matsumoto, Akiba and Murakami (1984) have detected diffuse emission in the 2–5 μm band, with an estimated energy density δ = 1.2.

Type
IV. Extragalactic Background Radiation and Cosmology
Information
Symposium - International Astronomical Union , Volume 139: The Galactic and Extragalactic Background Radiation , 1990 , pp. 406 - 407
Copyright
Copyright © Kluwer 1990 

References

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