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The cosmic microwave background was first predicted in 1948 by Ralph Alpher and Robert Herman, in a correction [16] they prepared for a paper by Alpher's PhD advisor George Gamow. [17] Alpher and Herman were able to estimate the temperature of the cosmic microwave background to be 5 K. [18]
1938: Walther Nernst re-estimates the cosmic ray temperature as 0.75 K. [2] 1946: The term "microwave" is first used in print in an astronomical context in an article "Microwave Radiation from the Sun and Moon" by Robert Dicke and Robert Beringer. 1946: Robert Dicke predicts a microwave background radiation temperature of 20 K (ref: Helge Kragh)
It is the current standard model of Big Bang cosmology, [1] as it is the simplest model that provides a reasonably good account of: the existence and structure of the cosmic microwave background; the large-scale structure in the distribution of galaxies; the observed abundances of hydrogen (including deuterium), helium, and lithium;
The discovery of cosmic microwave background radiation constitutes a major development in modern physical cosmology. In 1964, US physicist Arno Allan Penzias and radio-astronomer Robert Woodrow Wilson discovered the cosmic microwave background (CMB) , estimating its temperature as 3.5 K, as they experimented with the Holmdel Horn Antenna .
CMB spectral distortions are tiny departures of the average cosmic microwave background (CMB) frequency spectrum from the predictions given by a perfect black body.They can be produced by a number of standard and non-standard processes occurring at the early stages of cosmic history, and therefore allow us to probe the standard picture of cosmology.
The steady-state model attempted to explain the microwave background radiation as the result of light from ancient stars that has been scattered by galactic dust. However, the cosmic microwave background level is very even in all directions, making it difficult to explain how it could be generated by numerous point sources, and the microwave ...
Differences in the temperature of the cosmic background are smoothed by cosmic inflation, but they still exist. The theory predicts a spectrum for the anisotropies in the microwave background which is mostly consistent with observations from WMAP and COBE. [6] However, gravity alone may be sufficient to explain this homogeneity. [7]
A comparison of the sensitivity and resolution of WMAP with COBE and Penzias and Wilson's telescope, simulated data [1]. This list is a compilation of experiments measuring the cosmic microwave background (CMB) radiation anisotropies and polarization since the first detection of the CMB by Penzias and Wilson in 1964.
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