Non-Gaussian temperature fluctuations in the cosmic microwave background sky from a random Gaussian density field

Details Non-Gaussian temperature fluctuations in the cosmic microwave background sky from a random Gaussian density field Non-Gaussian temperature fluctuations in the cosmic microwave background sky from a random Gaussian density field

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...375..439s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 375, July 10, 1991, p. 439-442. Research supported by Ministero della Ricer

Astronomy and Astrophysics

Astrophysics

40

Normal Density Functions, Relic Radiation, Temperature Distribution, Distribution Functions, Galactic Clusters, Random Processes, Statistical Distributions

Scientific paper

It is pointed out that the cosmic microwave background (CMB) temperature fluctuations, observed in the microwave sky with a large antenna beam, may not be Gaussian distributed, even if the primordial matter density fluctuations constitute a random Gaussian field. This effect is due to a dominance of low-order multipoles of the CMB anisotropy pattern and is then relevant for galaxy formation models with large-scale power, which produce CMB angular anisotropies through the familiar Sachs-Wolfe effect. Emphasis is given to the most popular case of a flat universe with scale-invariant, Gaussian distributed density fluctuations. In this case 30 percent of the cosmic observers would reject the hypothesis that CMB temperature fluctuations in their own microwave sky are Gaussian distributed at least at the 99 percent confidence level. Numerical bounds are given for the skewness and kurtosis of the sky pixel temperature fluctuation distribution.

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