University of Århus lunch talk, May 11, 2007

Large angle CMB anomalies and local structures

Large angle CMB anomalies and local structures

Syksy RäsänenCERN

Syksy RäsänenCERN

University of Århus lunch talk, May 11, 2007

WMAP: from one year to threeWMAP: from one year to three

University of Århus lunch talk, May 11, 2007

Ecliptic North-SouthEcliptic North-South

University of Århus lunch talk, May 11, 2007

WMAP1(Copi et al., http://www.phys.cwru.edu/projects/mpvectors/)

WMAP123

WMAP1(Copi et al., http://www.phys.cwru.edu/projects/mpvectors/)

WMAP123

Quadrupole and octopoleQuadrupole and octopole

University of Århus lunch talk, May 11, 2007

CMB analysisCMB analysisTemperature anisotropy

Anisotropy correlation

Temperature anisotropy

Anisotropy correlation

€

ΔT

T(θ,ϕ ) = alm

l,m∑ Ylm (θ,ϕ ) ≡ Tl (θ,ϕ )

l∑

€

ΔT

T(r n )

ΔT

T(r n ') = Cl

2l +1

4πPl (cosθ)

l∑

Cl =1

2l +1alm

2

m∑

€

Tl = Al ∏i=1

l

(r v (l ,i) ⋅

r e )

University of Århus lunch talk, May 11, 2007

StatisticsStatistics North-south anisotropy

Power asymmetry unlikely at 99.7% in WMAP1 (l=2-40), 87% in COBE-DMR. (Eriksen et al., astro-ph/0307507)

The WMAP1 “blips” in the power spectrum are associated with anomalous directions. (Hansen et al., astro-ph/0404206)

For WMAP123, dipolar modulation significant at 99% (frequentist) or 1:4 to 6 (78-83%, Bayesian). (Eriksen et al., astro-ph/0701089)

Planarity of l=2+3 WMAp123: Odds of 1:24 to 47 (96-98%, Bayesian). (Magueijo and Sorkin, astro-

ph/0604410)

Alignment of l=2+3 WMAP1: 99.4-99.6%, WMAP123: 99.6%. (Copi et al.,, astro-ph/0605135)

Correlation of l=2+3 with the ecliptic WMAP1: 98.3-99.8%, WMAP123: 89.7%. (Copi et al.,, astro-ph/0605135)

Correlation of l=2+3 with the dipole WMAP1: 94-96%, WMAP123: 93%. (Copi et al.,, astro-ph/0605135)

North-south anisotropy Power asymmetry unlikely at 99.7% in WMAP1 (l=2-40), 87% in

COBE-DMR. (Eriksen et al., astro-ph/0307507)

The WMAP1 “blips” in the power spectrum are associated with anomalous directions. (Hansen et al., astro-ph/0404206)

For WMAP123, dipolar modulation significant at 99% (frequentist) or 1:4 to 6 (78-83%, Bayesian). (Eriksen et al., astro-ph/0701089)

Planarity of l=2+3 WMAp123: Odds of 1:24 to 47 (96-98%, Bayesian). (Magueijo and Sorkin, astro-

ph/0604410)

Alignment of l=2+3 WMAP1: 99.4-99.6%, WMAP123: 99.6%. (Copi et al.,, astro-ph/0605135)

Correlation of l=2+3 with the ecliptic WMAP1: 98.3-99.8%, WMAP123: 89.7%. (Copi et al.,, astro-ph/0605135)

Correlation of l=2+3 with the dipole WMAP1: 94-96%, WMAP123: 93%. (Copi et al.,, astro-ph/0605135)

University of Århus lunch talk, May 11, 2007

Possible physical originsPossible physical origins1) Primordial perturbations

Seeing the start of inflation Fundamental anisotropy

2) Last scattering surface3) 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 surface3) 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 CMBLocal 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

€

ΔT

T(θ,ϕ ) = −2 dη∂ηφ(1)(η ,

r r (η ))∫

€

ΔT

T(θ,ϕ ) = −2 dη∂ηφ(2)(η ,

r r (η ))∫

€

ΔT

T(θ,ϕ ) =

?

− 2 dη∂ηφ(NL )(η ,r r (η ))∫

University of Århus lunch talk, May 11, 2007

Ecliptic frame (McClure and Dyer, astro-ph/0703556)

CMB dipole frame

Ecliptic frame (McClure and Dyer, astro-ph/0703556)

CMB dipole frame

The local expansion rateThe local expansion rate

University of Århus lunch talk, May 11, 2007

SummarySummary 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.