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IRAS observations of the diffuse infrared background
Hauser, M. G.; Gillett, F. C.; Low, F. J.; Gautier, T. N.; Beichman, C. A.; Neugebauer, G.; Aumann, H. H.; Baud, B.; Boggess, N.; Emerson, J. P.; Houck, J. R.; Soifer, B. T.; Walker, R. G.
AA(NASA, Goddard Space Flight Center, Greenbelt, MD), AB(Kitt Peak National Observatory, Tucson, AZ), AC(Steward Observatory, Tucson, AZ), AD(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AE(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AF(California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA), AG(California Institute of Technology, Pasadena, CA), AH(Groningen, Rijksuniversiteit, Groningen, Netherlands), AI(NASA, Washington, DC), AJ(Queen Mary College, London, England)
Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 278, March 1, 1984, p. L15-L18. (ApJL Homepage)
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NASA/STI Keywords:
Background Radiation, Diffuse Radiation, Infrared Astronomy, Interplanetary Dust, Brightness, Emission Spectra, Infrared Astronomy Satellite
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IRAS data reveal bright emission from interplanetary dust which dominates the celestial background at 12, 25, and 60 microns except near the galactic plane. At 100 microns, interplanetary dust emission is prominent only near the ecliptic plane; diffuse galactic emission is found over the rest of the sky. At the galactic poles, the observed brightness implies that A(v) is likely to be of order 0.1 mag. The angular variation of the zodiacal emission in the ecliptic plane and in the plane at elongation 90 deg, and an annual modulation of the ecliptic pole brightness, are generally consistent with previously determined interplanetary dust distributions.

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