Hostname: page-component-848d4c4894-wg55d Total loading time: 0 Render date: 2024-05-16T19:48:12.163Z Has data issue: false hasContentIssue false
  • English
  • Français

Small Scale Fluctuations in the Microwave Background Radiation Associated with the Formation of Galaxies

Published online by Cambridge University Press:  14 August 2015

R. A. Sunyaev
R. A. Sunyaev*
Affiliation:
Space Research Institute, USSR Academy of Sciences, Moscow, USSR.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

According to current ideas, massive extragalactic systems such as galaxies and clusters of galaxies formed as a result of the growth of small fluctuations in density and velocity which were present in the early stages of expansion of the Universe under the influence of gravitational instability. According to the hot model of the Universe at the epoch corresponding to a redshift z ≈ 1500, recombination of primaeval hydrogen took place and as a result the optical depth of the Universe to Thomson scattering decreased abruptly from about 1000 to 1 - the Universe became transparent. Therefore the observed angular distribution of the microwave background radiation (MWBR) contains information about inhomogeneities in its spatial distribution at a redshift z ∼ 1000. Silk (1968) was the first to note that this “photograph” of the Universe at the epoch of recombination must be enscribed with fluctuations associated with perturbations in the space density and velocity of motion of matter which will later lead to the formation of galaxies and clusters of galaxies.

Type
VI. Microwave Background Radiation
Information
Symposium - International Astronomical Union , Volume 74: Radio Astronomy and Cosmology , 1977 , pp. 327 - 334
Copyright
Copyright © Reidel 1977 

References

Literature

Anile, A.M., Danese, L., De Zotti, G. and Motta, S., 1976. Astrophys. J, 205, L59.Google Scholar
Arons, J. and Wingert, D., 1972. Astrophys. J., 177, 1.CrossRefGoogle Scholar
Carpenter, R.L., Gulkis, S. and Sato, H., 1973. Astrophys. J., 182, L61.CrossRefGoogle Scholar
Chibisov, G.V., 1972. Astron. Zh., 49, 286.Google Scholar
Chibisov, G.V. and Ozernoi, L.M., 1969. Astrophys. Letters, 3, 189.Google Scholar
Conklin, E.K. and Bracewell, R.N., 1967. Phys. Rev. Letters, 18, 614.CrossRefGoogle Scholar
Doroshkevich, A.G., Longair, M.S. and Zeldovich, Ya.B., 1970. Mon. Not. R. astr. Soc., 147, 139.Google Scholar
Gull, S.F. and Northover, K.J.E., 1976. Nature (in press).Google Scholar
Komberg, B.V. and Sunyaev, R.A., 1971. Astron. Zh., 48, 235.Google Scholar
Longair, M.S. and Sunyaev, R.A., 1969. Nature, 223, 719.Google Scholar
Parijskij, Yu.N., 1972. Astron. Zh., 49, 1322.Google Scholar
Parijskij, Yu.N., 1973. Astron. Zh., 50, 453.Google Scholar
Peebles, P.J.E., 1968. Astrophys. J., 162, 815.Google Scholar
Peebles, P.J.E. and Yu, I.T., 1970. Astrophys. J., 162, 815.CrossRefGoogle Scholar
Silk, J., 1968. Astrophys. J., 151, 459.Google Scholar
Stankevich, K.S., 1974. Astron. Zh., 51, 216.Google Scholar
Sunyaev, R.A. and Zeldovich, Ya.B., 1970. Astrophys. and Space Science, 7, 20.Google Scholar
Sunyaev, R.A. and Zeldovich, Ya.B., 1972. Comments Astrophys. and Sp. Phys., 4, 173.Google Scholar
Weinberg, S., 1972. “Gravitation and Cosmology”, Wiley, New York.Google Scholar
Zeldovich, Ya.B., Kurt, V.G. and Sunyaev, R.A., 1968. ZhETP., 55, 278.Google Scholar