Hostname: page-component-cd9895bd7-hc48f Total loading time: 0 Render date: 2024-12-26T04:30:17.186Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

REFERENCES

Bond, J.R. Carr, B.J., and Hogan, C.J. 1986, Astrophys. J., 306, 428.Google Scholar
Hoffman, W., and Lemke, D. 1978, Astron. Astrophys., 68, 389.Google Scholar
Matsumoto, T., Akiba, M., and Murakami, H. 1984, in Advances in Space Research, ed. Bignami, G.F. and Sunyaev, R.A. (Oxford: Pergamon), 1.Google Scholar
Partridge, R.B., and Peebles, P.J.E. 1967, Astrophys. J., 148, 377.Google Scholar
Rephaeli, Y. 1988, Comments on Astrophys., 12, 265.Google Scholar
Rephaeli, Y., and Schlickeiser, R. 1988, Astron. Astrophys., 194, 99.Google Scholar
Rephaeli, Y., Gruber, D.E., and Rothschild, R.E. 1987, Astrophys. J., 320, 139.Google Scholar
Rephaeli, Y., Gruber, D.E. 1988, Astrophys. J., 333, 133.Google Scholar
Rowan-Robinson, M. 1986, 219, 737.Google Scholar
Schlickeiser, R. and Harwit, M. 1982, Astron. Astrophys., 107, 186.Google Scholar
Stecker, F.W., Puget, J.L., and Fazio, G.G. 1977, Astrophys. J. (Letters), 214, L51.Google Scholar
Vallee, J.P., Broten, N.W., and MacLeod, J.M. 1987, Astrophys. Lett., 25, 181.Google Scholar