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WMAP Cosmology

WMAP Cosmology. Courtesy of NASA/WMAP Science Team map.gsfc.nasa.gov. Before And After The First Light. From COBE to WMAP. 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. 94 GHz, 0.21 o ,   1.4 mK/  N obs.

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WMAP Cosmology

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  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, 0.82o ,  6 mK/Nobs 33 GHz, 0.62o ,  3 mK/Nobs 41 GHz, 0.49o ,  2 mK/Nobs 94 GHz, 0.21o ,   1.4 mK/Nobs 61 GHz, 0.33o ,   1.4 mK/Nobs Galactic mask from the lowest frequency Nobs  103

  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 Adiabatic Isocurvature

  8. Cosmological Parameters Basic Analysis: h, ns, k dns/dk, b h2, m h2, 8,  Extension: , m ,wDE, r 2,WMAP, WMAP+ACBAR+CBI+2dF+Lyman b h2 =0.0220.001,0.0224 0.0009 +0.008 m h2 =0.140.01,0.135 -0.009 h=0.710.06,0.71 +0.04 -0.03  =0.200.07,0.17 0.06 ns=0.910.06,0.930.03 k dns/dk =...,-0.031 +0.016 -0.017 8=0.9 0.1,0.83 +0.09 -0.08

  9. Extension:  WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/MPc): =1.020.02 Extension: m WMAP+ACBAR+CBI+2dF: h2=imi/93.5 eV < 0.0076 m <0.23 eV Extension: wDE WMAP+ACBAR+CBI+HST+SNIa+2dF: wDE < -0.78 Extension: r WMAP+ACBAR+CBI+2dF+infl.cons.rel.: r < -0.71

  10. The Limits On Non-Gaussianity Departure from Gaussianity at 2th order: Y =YL+fNL(YL2-<YL2>) The simplest inflationary scenario predicts fNL' 10-1 WMAP: -58< fNL< -134

  11. Reionisation ClTexp(-2) on l > lrh ClT,TE,E,Bon l < lrh 0.20

  12. 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?

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

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

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