1. WMAP Cosmology Courtesy of NASA/WMAP Science Team map.gsfc.nasa.gov

2. Before And After The First Light

3. From COBE to WMAP

4. WMAP Maps 23 GHz, 0.82 o,  6 mK/  N obs 33 GHz, 0.62 o,  3 mK/  N obs 41 GHz, 0.49 o,  2 mK/  N obs 61 GHz, 0.33 o,  1.4 mK/  N obs 94 GHz, 0.21 o,  1.4 mK/  N obs Galactic mask from the lowest frequency N obs 10 3

5. The CMB Angular Power Spctrum

6. Throwing Pebbles In The Primordial Pond Homogeneity & Isotropy Black Body Spectrum + + +

7. Understanding The Sound Of The Early Universe Isocurvature Adiabatic

11. Cosmological Parameters Basic Analysis: h, n s, k  dn s /dk,  b h 2,  m h 2,  8,  2 ,WMAP, WMAP+ACBAR+CBI+2dF+Lyman  Extension: , m ,w DE, r h=0.71  0.06, 0.71 +0.04 n s =0.91  0.06, 0.93  0.03 k  dn s /dk =..., -0.031 +0.016 -0.017  b h 2 =0.022  0.001, 0.0224  0.0009  m h 2 =0.14  0.01, 0.135 +0.008 -0.009  8 =0.9  0.1, 0.83 +0.09 -0.08 -0.03  =0.20  0.07, 0.17  0.06

12. Extension:  WMAP+ACBAR+CBI+HST+SNIa+(H 0 >50 km/sec/MPc):  =1.02  0.02 Extension: m  Extension: w DE Extension: r WMAP+ACBAR+CBI+2dF:   h 2 =  i m i /93.5 eV < 0.0076  m  <0.23 eV WMAP+ACBAR+CBI+HST+SNIa+2dF: w DE < -0.78 WMAP+ACBAR+CBI+2dF+infl.cons.rel.: r < -0.71

13. The Limits On Non-Gaussianity  =  L +f NL (  L 2 - ) WMAP: -58< f NL < -134 Departure from Gaussianity at 2 th order: The simplest inflationary scenario predicts f NL ' 10 -1

14. Reionisation C l T  exp(-2  ) on l > l rh C l T,TE,E,B  on l < l rh  0.20

15. Open Problems: The Early Universe Initial conditions mostly adiabatic, Gaussian, scale-invariant, consistent with the simplest inflationary scenario, but that remains effective. Is the spectral index really running? What does it mean? Can we have a better limit on non-Gaussianity? Can we detect primordial gravitational waves? Can we hope to fix inflation into a coherent supersymmetric context?

16. Open Problems: Concordance Model An happy review of the Cosmological Constant Problem Log! nicely 96% Dark, with Cosmological Constant Shall we detect WIMPS eventually? Should we repeat the Einstein greatest blunder?

17. The CMB Future: Challenging The Concordance Imaging on all relevant CMB scales (Planck) TE modes cosmological polarisation, large scales (Planck) B modes cosmological polarisation, if r>30% (Planck) E modes cosmological polarisation, large scales (Planck) More...a CMB polarisation satellite? Dark Matter & Energy Properties (Planck, SNAP,ALMA) Needed: E modes cosmological polarisation, small scales (Planck, Quest,...) TE modes cosmological polarisation, small scales (Planck, Quest,...)