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WMAP 5-Year Observations:

Cosmological Interpretation

Eiichiro Komatsu University of Texas at Austin CITA, March 11, 2008

WMAP 5-Year Papers

Hinshaw et al. , “ Data Processing, Sky Maps, and Basic Results ”

Hill et al. , “ Beam Maps and Window Functions ” 0803.

Gold et al. , “ Galactic Foreground Emission ” 0803.

Wright et al. , “ Source Catalogue ” 0803.

Nolta et al. , “ Angular Power Spectra ” 0803.

Dunkley et al. , “ Likelihoods and Parameters from the WMAP data ” 0803.

Komatsu et al ., “ Cosmological Interpretation ” 0803.

WMAP 5-Year Press Release

On March 7, 2008

Evidence for the cosmic neutrino background from the WMAP data alone

Instantaneous reionization at zreion=6 is excluded at the 3.5 sigma level

The tightest constraints on inflation models to date

WMAP 5-Year Data

Hinshaw et al.

Hinshaw et al.

Improved Data/Analysis

Improved Beam Model

5 years of the Jupiter data, combined with the extensive physical optics modeling, reduced the beam uncertainty by a factor of 2 to 4.

Improved Calibration

Improved algorithm for the gain calibration from the CMB dipole reduced the calibration error from 0.5% to 0.2%

More Polarization Data Usable for Cosmology

We use the polarization data in Ka band. (We only used Q and V bands for the 3-year analysis.)

The 5-Year C

l

Nolta et al. Cosmic variance limited to l= Much improved measurement of the 3rd peak!

The 5-Year C

l

Nolta et al. Note consistency around the 3rd- peak region

Adding Polarization in Ka:

Passed the Null Test

Hinshaw et al. Errors include cosmic variance Black Symbols are upper limits

(Ka - QV)/

Adding Polarization in Ka:

Passed the Null Test!!

Optical Depth measured from the EE power spectrum:

Tau(5yr)=0.087 +/- 0.

Tau(3yr)=0.089 +/- 0. (Page et al.; QV only)

3-sigma to 5-sigma!

Tau form the null map (Ka- QV) is consistent with zero Hinshaw et al.

Cosmic Neutrino Background

How do neutrinos affect CMB?

They change the radiation-to-matter ratio. The larger the number of neutrino species is, the later the matter-radiation equality, zequality , becomes.

So, this effect is degenerate with the matter density.

Neutrino perturbations affect metric perturbations as well as the photon-baryon plasma, through which CMB anisotropy is affected.

CNB as seen in WMAP

Multiplicative phase shift is due to the change in zequality

Degenerate with Ωmh 2

Suppression is due to neutrino perturbations

Degenerate with ns

Additive phase shift is due to neutrino perturbations

No degeneracy (Bashinsky & Seljak 2004) Red: Neff=3. Blue: Neff= Δχ 2 =8.2 -> 99.5% CL Dunkley et al.

Cosmic/Laboratory

Consistency

From WMAP+BAO+SN (I will explain what BAO and SN are shortly)

Neff=4.4 +/- 1.

From the Big Bang Nucleosynthesis

Neff=2.5 +/- 0.

From the decay width of Z bosons measured in LEP

Nneutrino=2.984 +/- 0. Komatsu et al.

Testing Inflation

Is the observable universe flat?

Are the primordial fluctuations adiabatic?

Are the primordial fluctuations nearly Gaussian?

Is the power spectrum nearly scale invariant?

Is the amplitude of gravitational waves reasonable?