Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-03T01:39:13.498Z Has data issue: false hasContentIssue false
  • English
  • Français

Recent Results from the COBE Differential Microwave Radiometer

Published online by Cambridge University Press:  30 March 2016

C. L. Bennett
C. L. Bennett*
Affiliation:
Code 685, Laboratory for Astronomy and Solar Physics NASA Goddard Space Flight CenterGreenbelt, MD 20771U.S.A.

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.

The scientific objective of the COBE Differential Microwave Radiometer (DMR) investigation is to use the cosmic microwave background (CMB) radiation as a probe of cosmology. Stringent limits can be set on the amplitude of fluctuations of the potential energy at the surface of last scattering of the CMB photons. Large angular scale (>1 .) fluctuations in the gravitational potential energy are directly related to temperature anisotropies in the CMB by the Sachs-Wolfe Effect (Sachs & Wolfe 1967), which describes the gravitational redshift of photons as they are last scattered at a gravitational potential energy per unit mass, ϕ, giving δϕ/c2 = 3δT/T. The DMR instrument was described by Smoot et al. (1990), recent scientific results by Smoot et al. (1991a,b), and calibration by Bennett et al. (1991). The DMR consists of two independent radiometers at each of three frequencies: 31.5, 53, and 90 GHz. Each radiometer measures the difference in temperature between two 7. FWHM beams separated by 60.. The scanning pattern of the instrument causes all 60. separation pixel-pairs to be observed thousands of times.

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. 335 - 336
Copyright
Copyright © Kluwer 1992

References

REFERENCES

Bennett, C.L. et al. 1991, in preparation.Google Scholar
Bond, J.R. & Efstathiou, G. 1984, APJ, 285, L45.Google Scholar
Collins, C.B. & Hawking, S.W. 1973, MNRAS, 162, 307.CrossRefGoogle Scholar
Efstathiou, G., Sutherland, W.J., & Maddox, S.J. 1990, Nature, 348, 705.CrossRefGoogle Scholar
Maddox, S.J., Efstathiou, G., Sutherland, W., & Loveday, J. 1990, MNRAS, 242, 43.Google Scholar
Sachs, R.K. & Wolfe, A.M. 1967, APJ, 147, 73.Google Scholar
Smoot, G. et al. 1990, APJ, 360, 685.Google Scholar
Smoot, G.F. et al. 1991a, After the First Three Minutes, AIP Conf. Proc. 222, Holt, S. S., Bennett, C. L., & Trimble, V., eds., AIP, New York.Google Scholar
Smoot, G.F. et al. 1991b, APJ Lett, 371, L1.CrossRefGoogle Scholar