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Title:
Interpretation of the COBE FIRAS CMBR spectrum
Authors:
Wright, E. L.; Mather, J. C.; Fixsen, D. J.; Kogut, A.; Shafer, R. A.; Bennett, C. L.; Boggess, N. W.; Cheng, E. S.; Silverberg, R. F.; Smoot, G. F.; Weiss, R.
Affiliation:
AA(UCLA, Los Angeles, CA, US), AB(UCLA, Los Angeles, CA, US), AC(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AD(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AE(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AF(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AG(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AH(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AI(NASA. Goddard Space Flight Center, Greenbelt, MD, US), AJ(NASA. Goddard Space Flight Center, Greenbelt, MD, US)
Publication:
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 420, no. 2, p. 450-456 (ApJ Homepage)
Publication Date:
01/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
BACKGROUND RADIATION, BIG BANG COSMOLOGY, COSMIC RAYS, FAR INFRARED RADIATION, MICROWAVE SPECTRA, BACKGROUND NOISE, BLACK BODY RADIATION, CALIBRATING, COSMIC BACKGROUND EXPLORER SATELLITE, MATHEMATICAL MODELS, MICHELSON INTERFEROMETERS, SIGNAL DISTORTION
DOI:
10.1086/173576
Bibliographic Code:
1994ApJ...420..450W

Abstract

The cosmic microwave background radiation (CMBR) spectrum measured by the Far-Infrared Absolute Spectrophotometer (FIRAS) instrument on NASA's Cosmic Background Explorer (COBE) is indistinguishable from a blackbody, implying stringent limits on energy release in the early universe later than the time t = 1 yr after the big bang. We compare the FIRAS data to previous precise measurements of the cosmic microwave background spectrum and find a reasonable agreement. We discuss the implications of the absolute value of y is less than 2.5 x 10-5 and the absolute value of mu is less than 3.3 x 10-4 95% confidence limits found by Mather et al. (1994) on many processes occurring after t = 1 yr, such as explosive structure formation, reionization, and dissipation of small-scale density perturbations. We place limits on models with dust plus Population III stars, or evolving populations of IR galaxies, by directly comparing the Mather et al. spectrum to the model predictions.

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