WMAP Cosmology
Courtesy of
NASA/WMAP Science Team
map.gsfc.nasa.gov
Before And After The First Light
From COBE to WMAP
WMAP Maps
41 GHz, 0.49o ,
2
mK/Nobs
33 GHz, 0.62o ,
3
mK/Nobs
23 GHz, 0.82o ,
6
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
The CMB Angular Power Spctrum
Throwing Pebbles In The Primordial Pond
+
+
+
Homogeneity
& Isotropy
Black Body Spectrum
Understanding The Sound Of The Early Universe
Adiabatic
Isocurvature
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
m h2 =0.140.01, 0.135
h=0.710.06, 0.71
 =0.200.07, 0.17 0.06
ns=0.910.06, 0.930.03
k dns/dk =..., -0.031
8=0.9 0.1, 0.83
+0.008
-0.009
+0.04
-0.03
+0.016
+0.09
-0.08
-0.017
Extension: 
WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/MPc):
Extension: m
=1.020.02
WMAP+ACBAR+CBI+2dF:
h2=imi/93.5 eV < 0.0076 m <0.23 eV
Extension: wDE
WMAP+ACBAR+CBI+HST+SNIa+2dF:
Extension: r
wDE < -0.78
WMAP+ACBAR+CBI+2dF+infl.cons.rel.:
r < -0.71
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
Reionisation
ClTexp(-2) on l > lrh
ClT,TE,E,Bon l < lrh
0.20
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?
Open Problems: Concordance Model
nicely 96% Dark, with Cosmological Constant
Shall we detect WIMPS eventually?
Should we repeat the Einstein greatest blunder?
120
Log!
100
Planck Energy
Density
80
60
40
20
0
Cosmological
Constant Today
Electro-Weak
Symmetry
Breaking
An happy review of
the Cosmological
Constant Problem
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?