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The telescope is designed for observations in the microwave, millimeter-wave, and submillimeter-wave regions of the electromagnetic spectrum, with the particular design goal of measuring the faint, diffuse emission from the cosmic microwave background (CMB). [49]
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.
There is background radiation observed across all wavelength regimes, peaking in microwave, but also notable in infrared and X-ray regimes. Fluctuations in cosmic background radiation across regimes create parameters for the amount of baryonic matter in the universe [5]. See cosmic infrared background and X-ray background.
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.
Schematic representation of the spectral energy distribution of the DEBRA. The dependent quantity is the spectral radiance multiplied by wavelength, i.e. λL eλ.Legend: gamma-ray background (CGB), cosmic X-ray background (CXB), cosmic ultraviolet/optical background (CUVOB), cosmic infrared background (CIB), cosmic microwave background (CMB), and cosmic radio background (CRB)
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 .
Cosmic Background Explorer (COBE) 1989 1990 Space Earth orbit: 68-3000 200 frequencies (FIRAS) Bolometers CMB Spectrum; CMB Temperature; CIB spectrum; Temperature anisotropies; frequency power spectrum; solar system and galactic dust foregrounds. [10] [25] TRIS 1994 2001 Ground Campo Imperatore: 0.6, 0.82, 2.5 CMB frequency power spectrum [10 ...
The limit is set by the slowing effect of interactions of the protons with the microwave background radiation over long distances (≈ 160 million light-years). The limit is at the same order of magnitude as the upper limit for energy at which cosmic rays have experimentally been detected, although indeed some detections appear to have exceeded ...