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WMAP Cosmology

This content explores the significant advancements in cosmology through the transition from the COBE satellite to the WMAP mission. It discusses the Cosmic Microwave Background (CMB) data, including maps at various frequencies, and delves into cosmological parameters such as homogeneity, isotropy, and non-Gaussianity. The document raises critical questions about the early universe, the spectral index, dark matter, and the intricacies of the cosmological constant. Looking to the future, challenges and potential new missions are outlined, emphasizing the ongoing quest to enhance our understanding of the universe.

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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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