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The cosmic microwave background (CMB, CMBR), or relic radiation, is microwave radiation that fills all space in the observable universe. With a standard optical telescope , the background space between stars and galaxies is almost completely dark.
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)
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.
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.
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 Sunyaev–Zeldovich effect (named after Rashid Sunyaev and Yakov B. Zeldovich and often abbreviated as the SZ effect) is the spectral distortion of the cosmic microwave background (CMB) through inverse Compton scattering by high-energy electrons in galaxy clusters, in which the low-energy CMB photons receive an average energy boost during collision with the high-energy cluster electrons.
Already in 1967, Dennis Sciama predicted that the cosmic microwave background has a significant dipole anisotropy. [41] [42] In recent years, the CMB dipole has been tested, and the results suggest our motion with respect to distant radio galaxies [43] and quasars [44] differs from our motion with respect to the cosmic microwave background.
The cosmic microwave background radiation (CMBR), for example, is a weak microwave noise filling empty space which is a major source of information on cosmology's Big Bang theory of the origin of the Universe.