Non-Gaussian Probability Distribution for the CMB Angular Power Spectra?

TL;DR

This paper discusses non-Gaussian features in WMAP five-year data, suggesting that the observed signals are more likely due to Galactic foreground effects than cosmological perturbations.

Contribution

The paper provides a detailed analysis of non-Gaussian features in CMB data and offers a reinterpretation of recent findings, emphasizing foreground effects over primordial signals.

Findings

Non-Gaussian features are likely due to Milky Way foregrounds.

The detected signals probably do not originate from cosmological perturbations.

Insights from discussions suggest a foreground origin for the observed non-Gaussianity.

Abstract

This is my contribution to Proceedings of the International Workshop on Cosmic Structure and Evolution, September 23-25, 2009, Bielefeld, Germany. In my talk I presented some non-Gaussian features of the foreground reduced WMAP five year full sky temperature maps, which were recently reported in arXiv:0906.4954 paper by V.Vanchurin. And in these notes I first discuss the statistics behind this analysis in some detail. Then I describe invaluable insights which I got from discussions after my talk on the Workshop. And finally I explain why, in my current opinion, the signal detected in arXiv:0906.4954 can hardly have something to do with cosmological perturbations, but rather it presents a fancy measurement of the Milky Way angular width in the microwave frequency range.