000108833 001__ 108833
000108833 005__ 20190316234017.0
000108833 0247_ $$2doi$$a10.1111/j.1365-2966.2008.12901.x
000108833 02470 $$2DAR$$a11866
000108833 02470 $$2ISI$$a000253980700030
000108833 037__ $$aARTICLE
000108833 245__ $$aNon-Gaussianity analysis on local morphological measures of WMAP data
000108833 269__ $$a2008
000108833 260__ $$c2008
000108833 336__ $$aJournal Articles
000108833 520__ $$aThe decomposition of a signal on the sphere with the steerable wavelet constructed from the second Gaussian derivative gives access to the orientation, signed-intensity and elongation of the signal’s local features. In the present work, the non-Gaussianity of the Wilkinson Microwave Anisotropy Probe (WMAP) temperature data of the cosmic microwave background (CMB) is analysed in terms of the first four moments of the statistically isotropic random fields associated with these local morphological measures, at wavelet scales corresponding to angular sizes between 27.5 arcmin and 30° on the celestial sphere. While no detection is made either in the orientation analysis or in the elongation analysis, a strong detection is made in the excess kurtosis of the signed-intensity of the WMAP data. The non-Gaussianity is observed with a significance level below 0.5 per cent at a wavelet scale corresponding to an angular size around 10°, and confirmed at neighbouring scales. This supports a previous detection of an excess of kurtosis in the wavelet coefficient of the WMAP data with the axisymmetric Mexican hat wavelet. Instrumental noise and foreground emissions are not likely to be at the origin of the excess of kurtosis. Large-scale modulations of the CMB related to some unknown systematics are rejected as possible origins of the detection. The observed non-Gaussianity may therefore probably be imputed to the CMB itself, thereby questioning the basic inflationary scenario upon which the present concordance cosmological model relies. Taking the CMB temperature angular power spectrum of the concordance cosmological model at face value, further analysis also suggests that this non-Gaussianity is not confined to the directions on the celestial sphere with an anomalous signed-intensity.
000108833 6531_ $$acosmology
000108833 6531_ $$aCMB
000108833 6531_ $$awavelets on the sphere
000108833 6531_ $$aGaussianity analysis
000108833 6531_ $$aLTS2
000108833 700__ $$0240427$$g163268$$aWiaux, Y.
000108833 700__ $$aVielva, P.
000108833 700__ $$aBarreiro, R. B.
000108833 700__ $$aMartínez-González, E.
000108833 700__ $$0240428$$g120906$$aVandergheynst, P.
000108833 773__ $$j385$$tMon. Not. R. Astron. Soc.$$q939
000108833 8564_ $$uhttp://www.blackwellpublishing.com/journal.asp?ref=0035-8711$$zURL
000108833 8564_ $$uhttps://infoscience.epfl.ch/record/108833/files/wmapnongaus-arXiv-0706.2346v2.pdf$$zn/a$$s278058
000108833 909C0 $$xU10380$$0252392$$pLTS2
000108833 909CO $$ooai:infoscience.tind.io:108833$$qGLOBAL_SET$$pSTI$$particle
000108833 937__ $$aEPFL-ARTICLE-108833
000108833 973__ $$rREVIEWED$$sPUBLISHED$$aEPFL
000108833 980__ $$aARTICLE