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Cosmic microwave background spectral distortions – Fluctuations in the energy spectrum of the microwave background Cosmological perturbation theory – theory by which the evolution of structure is understood in the big bang model Pages displaying wikidata descriptions as a fallback
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 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 .
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)
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.
In 1964 the cosmic microwave background radiation was discovered as predicted by the Big Bang theory. 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.
Structure formation began some time after recombination, when the early universe cooled enough from expansion to allow the formation of stable hydrogen and helium atoms. [7]: 6 At this point the cosmic microwave background(CMB) is emitted; many careful measurements of the CMB provide key information about the initial state of the universe before structure formation.
Once photons decoupled from matter, they traveled freely through the universe without interacting with matter and constitute what is observed today as cosmic microwave background radiation (in that sense, the cosmic background radiation is infrared and some red black-body radiation emitted when the universe was at a temperature of some 3000 K ...