Cosmic microwave background radiation


Cosmic microwave
background radiation

June 2001

The Cosmic Microwave Background Radiation is a form of electromagnetic radiation that fills the whole of the universe. It has the characteristics of black body radiation at a temperature of 2.726 kelvins. It has a frequency in the microwave range.

Table of contents
1 Big Bang Evidence?
2 Features
3 Theory
4 Experiments
5 Skeptics
6 See also
7 Bibliography
8 References and external links

Big Bang Evidence?

This radiation is regarded as the best available evidence of the Big Bang theory -- it gives a snapshot of the Universe when the temperature dropped enough to allow electrons and protons to form hydrogen atoms, thus making the universe transparent to radiation. When it originated some 300,000 years after the Big Bang -- this point in time is generally known as the "last scattering surface" -- the temperature of the Universe was about 6000 K. Since then it has dropped because of the expansion of the Universe, which cools radiation inversely proportional to the fourth power of the Universe's scale length.

Features

One of the microwave background's most salient features is a high degree of isotropy. There are some anisotropies, the most pronounced of which is the dipole anisotropy at a level of about 10-4 at a scale of 180 degrees of arc. It is due to the motion of the observer against the CBR, which is some 700 km/s for the Earth.

Much smaller variations due to external physics also exist; the Sunyaev-Zel'dovic-Effect is one of the major factors here.

Even more interesting are anisotropies at a level of roughly 1/100000 and on a scale of a few arc minutes. Those very small variations correspond to the density fluctuations at the last scattering surface and give valuable information about the seeds for the large scale structures we observe now. These small-scale variations give observational constraints on the properties of universe, and are therefore one important test for cosmological models.

Theory

The CBR was predicted by George Gamow, Ralph Alpher, and Robert Hermann in the 1940s and was accidentally discovered in the 1964 by Penzias and Wilson, who received a Nobel Prize for this discovery. Since the cosmic microwave radiation is rather difficult to observe with ground-based instruments, CMB research makes increasing use of air and space-borne experiments.

Experiments

Of these experiments, the Cosmic Background Explorer (COBE) satellite that was flown in 1989-1996 is probably the most famous and which made the first detection of the large scale anisotropies (other than the dipole). In June 2001, NASA launched a second CBR space mission, WMAP, to make detailed measurements of the anisotropies over the full sky. Results from this mission provide a detailed measurement of the angular power spectrum down to degree scales, giving detailed constraints on various cosmological parameters. The results are broadly consistent with those expected from cosmic inflation as well as various other competing theories, and are available in detail at http://lambda.gsfc.nasa.gov/.

A third space mission, Planck, is to be launched in 2007. Unlike the previous two space missions, Planck is a collaboration between NASA and ESA (the European Space Agency).

Skeptics

Some researchers point out that the Sunyaev-Zel'dovich theory could account for the "concentrations" observed in the radiations's path to the detector from a uniform source. Here the universe was once superheated (nearly 14 billion years ago), the Sunyaev-Zel'dovich Effect's "condenses" the cosmic microwave background by collapsed structures containing baryons. This could mean that the particular original form of the energy contents of the Universe (and it associated conditions) before recombination is uniform (something that the big bang model does not account for fully).

See also

Bibliography

  • Seife, Charles BREAKTHROUGH OF THE YEAR: Illuminating the Dark Universe, Science 2003 302: 2038-2039
  • Partridge, R. B. "3K: The Cosmic Microwave Background Radiation". New York, Cambridge University Press, 1995.

References and external links




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