COSMOLOGICAL IMPLICATIONS OF THE CMB LARGE-SCALE STRUCTURE

• Main Author: Melia, Fulvio
• Other Authors: The University of Arizona
• Language: en
• Published: IOP PUBLISHING LTD 2014
• Online Access: http://hdl.handle.net/10150/615117; http://arizona.openrepository.com/arizona/handle/10150/615117

The Wilkinson Microwave Anisotropy Probe (WMAP) and {\it Planck} {\bf may have} uncovered several anomalies in the full cosmic microwave background (CMB) sky that {\bf could indicate} possible new physics driving the growth of density fluctuations in the early Universe. These include an unusually low power at the largest scales and an apparent alignment of the quadrupole and octopole moments. In a $\Lambda$CDM model where the CMB is described by a Gaussian Random Field, the quadrupole and octopole moments should be statistically independent. {\bf The emergence of these low probability features may simply be due to posterior selections from many such possible effects, whose occurrence would therefore not be as unlikely as one might naively infer. If this is not the case, however, and if these features are not due to effects such as foreground contamination, their combined statistical significance would be equal to the product of their individual significances.} In the absence of such extraneous factors, {\bf and ignoring the biasing due to posterior selection, the missing large-angle correlations would have a probability as low as $\sim 0.1\%$ and the low-$l$ multipole alignment would be unlikely at the $\sim 4.9\%$ level; under the least favourable conditions, their simultaneous observation in the context of the standard model could then be likely at only the $\sim 0.005\%$ level.} In this paper, {\bf we explore the possibility that these features are indeed anomalous, and} show that the corresponding probability of CMB multipole alignment in the $R_{\rm h}=ct$ Universe {\bf would then be} $\sim 7-10\%$, depending on the number of large-scale Sachs-Wolfe induced fluctuations. Since the low power at the largest spatial scales is reproduced in this cosmology without the need to invoke cosmic variance, the overall likelihood of observing both of these features in the CMB is $\geq 7\%$, {\bf much more likely than in $\Lambda$CDM, if the anomalies are real.} The key physical ingredient responsible for this difference is the existence in the former of a maximum fluctuation size at the time of recombination, which is absent in the latter because of inflation.