000191153 001__ 191153
000191153 005__ 20181203023339.0
000191153 0247_ $$2doi$$a10.1051/0004-6361/201219793
000191153 022__ $$a0004-6361
000191153 02470 $$2ISI$$a000325211900010
000191153 037__ $$aARTICLE
000191153 245__ $$aRemoval of two large-scale cosmic microwave background anomalies after subtraction of the integrated Sachs-Wolfe effect
000191153 260__ $$aLes Ulis Cedex A$$bEdp Sciences S A$$c2013
000191153 269__ $$a2013
000191153 300__ $$a15
000191153 336__ $$aJournal Articles
000191153 520__ $$aContext. Although there is currently a debate over the significance of the claimed large-scale anomalies in the cosmic microwave background (CMB), their existence is not totally dismissed. In parallel to the debate over their statistical significance, recent work has also focussed on masks and secondary anisotropies as potential sources of these anomalies. Aims. In this work we investigate simultaneously the impact of the method used to account for masked regions as well as the impact of the integrated Sachs-Wolfe (ISW) effect, which is the large-scale secondary anisotropy most likely to affect the CMB anomalies. In this sense, our work is an update of previous works. Our aim is to identify trends in CMB data from different years and with different mask treatments. Methods. We reconstruct the ISW signal due to 2 Micron All-Sky Survey (2MASS) and NRAO VLA Sky Survey (NVSS) galaxies, effectively reconstructing the low-redshift ISW signal out to z similar to 1. We account for regions of missing data using the sparse inpainting technique. We test sparse inpainting of the CMB, large scale structure and ISW and find that it constitutes a bias-free reconstruction method suitable to study large-scale statistical isotropy and the ISW effect. Results. We focus on three large-scale CMB anomalies: the low quadrupole, the quadrupole/octopole alignment, and the octopole planarity. After sparse inpainting, the low quadrupole becomes more anomalous, whilst the quadrupole/octopole alignment becomes less anomalous. The significance of the low quadrupole is unchanged after subtraction of the ISW effect, while the trend amongst the CMB maps is that both the low quadrupole and the quadrupole/octopole alignment have reduced significance, yet other hypotheses remain possible as well (e. g. exotic physics). Our results also suggest that both of these anomalies may be due to the quadrupole alone. While the octopole planarity significance is reduced after inpainting and after ISW subtraction, however, we do not find that it was very anomalous to start with.
000191153 6531_ $$acosmic background radiation
000191153 6531_ $$aCosmology: theory
000191153 6531_ $$aearly Universe
000191153 6531_ $$alarge-scale structure of Universe
000191153 6531_ $$aCosmology: observations
000191153 6531_ $$amethods: statistical
000191153 700__ $$0245766$$aRassat, A.$$g214582$$uEcole Polytech Fed Lausanne, Observ Sauverny, Astrophys Lab, CH-1290 Versoix, Switzerland
000191153 700__ $$aStarck, J.-L.$$uCEA Saclay, Lab AIM, UMR CEA CNRS Paris 7, Irfu,Serv Astrophys, F-91191 Gif Sur Yvette, France
000191153 700__ $$aDupe, F.-X.
000191153 773__ $$j557$$tAstronomy & Astrophysics
000191153 909C0 $$0252365$$pLASTRO$$xU10933
000191153 909CO $$ooai:infoscience.tind.io:191153$$pSB$$particle
000191153 917Z8 $$x103317
000191153 937__ $$aEPFL-ARTICLE-191153
000191153 973__ $$aEPFL$$rREVIEWED$$sPUBLISHED
000191153 980__ $$aARTICLE