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WMAP Cosmology
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WMAP Cosmology Courtesy of NASA/WMAP Science Team map.gsfc.nasa.gov
description
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. - PowerPoint PPT Presentation
Transcript of 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, 0.82o , 6 mK/Nobs
33 GHz, 0.62o , 3 mK/Nobs
41 GHz, 0.49o , 2 mK/Nobs
61 GHz, 0.33o ,
1.4 mK/Nobs
94 GHz, 0.21o ,
1.4 mK/Nobs
Galactic mask from the lowest frequencyNobs 103
The CMB Angular Power Spctrum
Throwing Pebbles In The Primordial Pond
Homogeneity& Isotropy
Black Body Spectrum
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Understanding The Sound Of The Early Universe
Isocurvature
Adiabatic
Cosmological Parameters
Basic Analysis: h, ns, k dns/dk, b h2, m h2, 8,
2,WMAP, WMAP+ACBAR+CBI+2dF+LymanExtension: , m ,wDE, r
h=0.710.06, 0.71+0.04
ns=0.910.06, 0.930.03k dns/dk =..., -0.031
+0.016-0.017
b h2 =0.0220.001, 0.0224 0.0009m h2 =0.140.01, 0.135
+0.008-0.009
8=0.9 0.1, 0.83+0.09-0.08
-0.03
=0.200.07, 0.17 0.06
Extension: WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/MPc):
=1.020.02Extension: m
Extension: wDE
Extension: r
WMAP+ACBAR+CBI+2dF:
h2=imi/93.5 eV < 0.0076 m <0.23 eV
WMAP+ACBAR+CBI+HST+SNIa+2dF:
wDE < -0.78
WMAP+ACBAR+CBI+2dF+infl.cons.rel.:
r < -0.71
The Limits On Non-Gaussianity
=L+fNL(L2-<L
2>)
WMAP: -58< fNL< -134
Departure from Gaussianity at 2th order:
The simplest inflationary scenario predicts fNL' 10-1
Reionisation
ClTexp(-2) on l > lrh
ClT,TE,E,Bon 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
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Planck EnergyDensity
CosmologicalConstant Today
Electro-WeakSymmetryBreaking
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?
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, ...)
