Hostname: page-component-848d4c4894-wg55d Total loading time: 0 Render date: 2024-05-22T01:07:13.907Z Has data issue: false hasContentIssue false
  • English
  • Français

The Cosmic Infrared Background

Published online by Cambridge University Press:  30 March 2016

M. G. Hauser
M. G. Hauser*
Affiliation:
Laboratory for Astronomy and Solar Physics Goddard Space Flight CenterGreenbelt, MD 20771

Abstract

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.

Cosmic infrared background radiation, expected to carry the radiative record of luminous objects since they first formed, has yet to be detected. The Diffuse Infrared Background Experiment (DIRBE) on the Cosmic Background Explorer (COBE) satellite is designed to search for this primeval background over the spectral range from 1 to 300 μm. Initial examination of data from this experiment show that foreground radiations from the solar system and Galaxy dominate the diffuse infrared sky brightness, with relative minima near 3.5 μm and in the submillimeter wavelength range. DIRBE measurements do not confirm some previous data from rockets and IRAS. Preliminary upper limits on the cosmic infrared background are generally above theoretical expectations for pregalactic and protogalactic sources, and substantially above estimated lower limits based upon observations of external galaxies. Careful foreground modeling is required to reduce these limits or identify an isotropic residual.

Type
Joint Discussions
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 291 - 296
Copyright
Copyright © Kluwer 1992

References

REFERENCES

Bond, J. R., Carr, B. J., and Hogan, C. J., 1986, Ap. J. 306, 428.CrossRefGoogle Scholar
Bond, J. R., Carr, B. J., and Hogan, C. J., 1991, Ap. J. 367, 420.CrossRefGoogle Scholar
Carr, B. J., Bond, J. R., and Hogan, C. J., 1991, “Cosmological Implications of COBE ”, in After the First Three Minutes, AIP Conference. Proceedings. 222, Holt, S. S., Bennett, C. L., and Trimble, V. (Eds.), pp. 187–201.CrossRefGoogle Scholar
Cowie, L. L., et al., 1990, Ap. J. (Lett.) 360, L1.CrossRefGoogle Scholar
Evans, D. C., 1983, SPIE Proc. 384, 82.CrossRefGoogle Scholar
Gulkis, S., Lubin, P. M., Meyer, S. S., and Silverberg, R. F., 1990, Sci. Am. 262, 132.CrossRefGoogle Scholar
Hacking, P. B. and Soifer, B. T., 1991, Ap. J. (Lett.) 367, L49.CrossRefGoogle Scholar
Harwit, M., 1970, Rivista del Nuovo Cimento Vol. II, 253.CrossRefGoogle Scholar
Hauser, M. G., et al., 1991, “The Diffuse Infrared Background: COBE and Other Observations”, in After the First Three Minutes, AIP Conference Proceedings 222, Holt, S. S., Bennett, C. L., and Trimble, V. (Eds.), pp. 161–178.CrossRefGoogle Scholar
Kaufman, M., 1976, Ap. Sp. Sci. 40, 369.CrossRefGoogle Scholar
Low, F. J. and Tucker, W. H., 1968, Phys. Rev. Lett. 22, 1538.CrossRefGoogle Scholar
Low, F. J. et al., 1984, Ap. J. (Lett.), 278, L19.CrossRefGoogle Scholar
Magner, T. J., 1987, Opt. Eng., 26, 264.CrossRefGoogle Scholar
Mather, J. C., 1982, Opt. Eng., 21, 769.CrossRefGoogle Scholar
Mather, J. C., et al., 1990, Proc. of IAU Colloquium 123 “Observatories in Earth Orbit and Beyond”, Kondo, Y. (ed.), Kluwer Acad. Publ., Dordrecht.Google Scholar
Matsumoto, T., 1990, “Infrared Extragalactic Background Light”, in The Galactic and Extragalactic Background Radiation, IAU Symposium 139, S., Bowyer and C., Leinert (Eds.), pp. 317–326.Google Scholar
Matsumoto, T., Akiba, M., and Murakami, H., 1988a, Ap. J. 332, 575.CrossRefGoogle Scholar
Matsumoto, T., et al. 1988b, Ap. J., 329, 567.CrossRefGoogle Scholar
Murdock, T. L., and Price, S. D., 1985, Astr. J. 90, 375.CrossRefGoogle Scholar
Noda, M. et al., 1991, “Rocket Observation of the Near-infrared Spectrum of the Sky” (preprint).Google Scholar
Partridge, R. B. and Peebles, P. J. E., 1967, Ap. J. 148, 377.CrossRefGoogle Scholar
Peebles, P. J. E., 1969, Phil. Trans. Royal Soc. London, A, 264, 279.Google Scholar