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Non-Gaussian Fluctuations

Wise, Mark B. (1988) Non-Gaussian Fluctuations. In: The Early Universe. NATO ASI series. Series C, Mathematical and physical sciences. Vol.219. Springer , Dordrecht, The Netherlands, pp. 215-238. https://resolver.caltech.edu/CaltechAUTHORS:20200928-152422345

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Abstract

Natural primordial mass density fluctuations are those for which the probability distribution, for the mass density fluctuations averaged over the horizon volume, is independent of time. This criterion determines the two-point correlation of the mass density fluctuations to have a Zeldovich power spectrum but allows for many types of higher correlations. If the connected higher correlations vanish the primordial fluctuations are Gaussian. In this case the probability distribution develops into a non-Gaussian one due to the non-linear time evolution. The nature of this non- Gaussian distribution and its effects on the large scale distribution of galaxies or clusters of galaxies and their large scale streaming velocities is explored. Next the possibility of natural primordial non-Gaussian fluctuations is examined. These can give rise to a very different large scale distribution of galaxies (or clusters of galaxies) than the Gaussian primordial fluctuations.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
https://doi.org/10.1007/978-94-009-4015-4_6DOIArticle
ORCID:
AuthorORCID
Wise, Mark B.0000-0002-9125-801X
Additional Information:© D. Reidel Publishing Company 1988.
Group:Caltech Theory
Other Numbering System:
Other Numbering System NameOther Numbering System ID
CALT-TH68-1410
Series Name:NATO ASI series. Series C, Mathematical and physical sciences
Record Number:CaltechAUTHORS:20200928-152422345
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200928-152422345
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105621
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:28 Sep 2020 22:38
Last Modified:28 Sep 2020 22:47

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