Radiation cosmic microwave background

R. W. Wilson, The cosmic microwave background radiation, pp. 113-33 in I.es Prix Nobel 1978. Almqvist Wiksell International, Stockholm 1979. A. A. Penzias, The origin of the elements, pp. 93-106 in Les Prix Nobel 1978 (also in Science 105, 549-54 (1979)). 

A. A. Penzias and R. W- Wilson (Holm-del) discovery of cosmic microwave background radiation. 

The primordial Li abundance was sought primarily because of its ability to constrain the baryon to photon ratio in the Universe, or equivalently the baryon contribution to the critical density. In this way, Li was able to complement estimates from 4He, the primordial abundance of which varied only slightly with baryon density. Li also made up for the fact that the other primordial isotopes, 2H (i.e. D) and 3He, were at that time difficult to observe and/or interpret. During the late 1990 s, however, measurements of D in damped Lyman alpha systems (high column-density gas believed to be related to galaxy discs) provided more reliable constraints on the baryon density than Li could do (e.g. [19]). Even more recently, the baryon density has been inferred from the angular power spectrum of the cosmic microwave background radiation, for example from the WMAP measurements [26]. We consider the role of Li plateau observations post WMAP. 

Cosmic microwave background radiation Fossil radiation surviving form the Big Bang with a black body temperature of 2.725 K. 

In consequence, the statistical characteristic temperature of relic radiation is fully determined in terms of relativistic invariant spectrum of the cosmic microwave background radiation and the distribution velocity function of radiating particles, i.e., is described with the following expression (compare with the results of reference (Einstein, 1965))... 

Anisotropic effects of the recorded frequency of cosmic microwave background radiation have been proposed for photon rest mass determination [20]. 

With reference to Table I, the energy usually flows frum higher levels to luwer levels—in a direction such ihut the entropy increases. Thus, cosmic microwave background radiation is defined as the ultimate heai sink. i,e il represents the ultimate in energy degradation with no lower form in which to be convened. 

T. Villela, N. Figueiredo, and C. A. Wuensche, Photon Mass Inferred from Cosmic Microwave Background Radiation Maxwell s Equations in three-Dimensional Space, Instituto Nacional de Pesquisas Espaciais, Brazil, circa 1994, pp. 65-73. 

Bob nods. The Universe is filled with the remnant heat from the Big Bang, the explosion that created our Universe somewhat over 10 billion years ago. The leftover heat we measure today is called the cosmic microwave background radiation. ... 

David Spergel, Gary Hinshaw, and Charles Bennett, NASA, The Cosmic microwave background radiation, http //map.gsfc.nasa.gov/html/cbr.html... 

Cosmic microwave background radiation The uniform background radiation in the microwave region of the spectrum that is observed in all directions in the sky. Its discovery added credence to the big bang model of the universe. 

De Bernadis, P and 35 others, 2000. A flat universe from high resolution maps of the cosmic microwave background radiation. Nature, 404, 955-9. 

Cosmic microwave background radiation (CMBR) is the oldest light we can see. It is a snapshot of how the universe looked in its early beginnings. First discovered in 1964, CMBR is composed of photons which we can see because of the atoms that formed when the universe cooled to 3000 K. Prior to that, after the Big Bang, the universe was so hot that the photons were scattered all over the universe, making the universe opaque. The atoms caused the photons to scatter less and the universe to become transparent to radiation. Since cooling to 3000K, the universe has continued to expand and cool. 

The neutrino analogue of the cosmic "microwave background radiation, i.e. a background radiation consisting of neutrinos. The CNB has not yet been detected it is thought that it would have a temperature of about 1.9 kelvin. 

The information concerning the constitution of the early Universe has increased tremendously during the past decade, mainly due to improved observations of the cosmic microwave background radiation (CMBR). The most important cosmological parameters (the total energy density, the part contained in baryonic matter, the part of nonbaryonic dark matter (DM), other components, etc.) have been determined with percent level accuracy as a result of projects completed in the first decade of the twenty-first century and now appear in tables of fundamental physical data (Amsler et al. 2008). 

Multipole fluctuation strength of the cosmic microwave background radiation as a function of the spherical harmonic index I. The location and the height of the first minimum favors a spatially flat Universe, while the level of the fluctuations in the higher multipoles (/ > 400) Indicates the presence of a low-density baryonic component (<5%). The measurements cover already the damping region (/ > 1,000). Wilkinson Microwave Anisotropy Probe (WMAP) data are displayed together with results of earlier balloon observations (Reprinted from Nolta et al. 2009 with kind permission of the first author, the WMAP Science Team, and AAS)... 

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