University of Århus lunch talk, May 11, 2007 Large angle CMB anomalies and local structures Syksy Räsänen CERN Syksy Räsänen CERN

University of Århus lunch talk, May 11, 2007 WMAP: from one year to three

University of Århus lunch talk, May 11, 2007 Ecliptic North-South

University of Århus lunch talk, May 11, 2007 WMAP1 (Copi et al., WMAP123 WMAP1 (Copi et al., WMAP123 Quadrupole and octopole

University of Århus lunch talk, May 11, 2007 CMB analysis Temperature anisotropy Anisotropy correlation Temperature anisotropy Anisotropy correlation

University of Århus lunch talk, May 11, 2007 Statistics  North-south anisotropy Power asymmetry unlikely at 99.7% in WMAP1 (l=2-40), 87% in COBE-DMR. (Eriksen et al., astro-ph/ ) The WMAP1 “blips” in the power spectrum are associated with anomalous directions. (Hansen et al., astro-ph/ ) For WMAP123, dipolar modulation significant at 99% (frequentist) or 1:4 to 6 (78-83%, Bayesian). (Eriksen et al., astro-ph/ )  Planarity of l=2+3 WMAp123: Odds of 1:24 to 47 (96-98%, Bayesian). (Magueijo and Sorkin, astro- ph/ )  Alignment of l=2+3 WMAP1: %, WMAP123: 99.6%. (Copi et al.,, astro-ph/ )  Correlation of l=2+3 with the ecliptic WMAP1: %, WMAP123: 89.7%. (Copi et al.,, astro-ph/ )  Correlation of l=2+3 with the dipole WMAP1: 94-96%, WMAP123: 93%. (Copi et al.,, astro-ph/ )  North-south anisotropy Power asymmetry unlikely at 99.7% in WMAP1 (l=2-40), 87% in COBE-DMR. (Eriksen et al., astro-ph/ ) The WMAP1 “blips” in the power spectrum are associated with anomalous directions. (Hansen et al., astro-ph/ ) For WMAP123, dipolar modulation significant at 99% (frequentist) or 1:4 to 6 (78-83%, Bayesian). (Eriksen et al., astro-ph/ )  Planarity of l=2+3 WMAp123: Odds of 1:24 to 47 (96-98%, Bayesian). (Magueijo and Sorkin, astro- ph/ )  Alignment of l=2+3 WMAP1: %, WMAP123: 99.6%. (Copi et al.,, astro-ph/ )  Correlation of l=2+3 with the ecliptic WMAP1: %, WMAP123: 89.7%. (Copi et al.,, astro-ph/ )  Correlation of l=2+3 with the dipole WMAP1: 94-96%, WMAP123: 93%. (Copi et al.,, astro-ph/ )

University of Århus lunch talk, May 11, 2007 Possible physical origins 1) Primordial perturbations  Seeing the start of inflation  Fundamental anisotropy 2) Last scattering surface 3) Passage between LSS and the local universe  Non-trivial topology  Global anisotropy/inhomogeneity 4) Local universe  Correlation with the source of the dipole 5) Solar system  Dust? 1) Primordial perturbations  Seeing the start of inflation  Fundamental anisotropy 2) Last scattering surface 3) Passage between LSS and the local universe  Non-trivial topology  Global anisotropy/inhomogeneity 4) Local universe  Correlation with the source of the dipole 5) Solar system  Dust?

University of Århus lunch talk, May 11, 2007 Local structures and the CMB  Linear cosmology: the Integrated Sachs-Wolfe Effect  Non-linear cosmology: the Rees-Sciama effect  Non-linear local structures: the local RS effect, the Moving Cluster of Galaxies effect  Linear cosmology: the Integrated Sachs-Wolfe Effect  Non-linear cosmology: the Rees-Sciama effect  Non-linear local structures: the local RS effect, the Moving Cluster of Galaxies effect

University of Århus lunch talk, May 11, 2007 Ecliptic frame (McClure and Dyer, astro-ph/ ) CMB dipole frame Ecliptic frame (McClure and Dyer, astro-ph/ ) CMB dipole frame The local expansion rate

University of Århus lunch talk, May 11, 2007 Summary  Breakdown of statistical anisotropy is the most significant anomaly in the CMB data.  Quadrupole and octopole are correlated with each other.  Anomalies extend to (at least) l=40.  Correlations with ecliptic, equinox and CMB dipole.  Quadrupole+octopole seems to be correlated with the local expansion rate, which points to the influence of local structures.  Breakdown of statistical anisotropy is the most significant anomaly in the CMB data.  Quadrupole and octopole are correlated with each other.  Anomalies extend to (at least) l=40.  Correlations with ecliptic, equinox and CMB dipole.  Quadrupole+octopole seems to be correlated with the local expansion rate, which points to the influence of local structures.