Charley Lineweaver UNSW

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Charley Lineweaver UNSW CMB 2 Feb 6
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COSMOLOGICAL PARAMETERS
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What are cosmological parameters?
Background
Bumps
Wcdm
Wm
WL
Quantum fluctuations
At
As
Wn
Ho
Wk
TCMB
nt
ns
to
w
galaxies clusters large scale structure
FRW metric Friedman Equation
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1997
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Cl
Radiation dominated
Matter dominated
recombination
Large scales
Small scales
Lineweaver 1997
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Carroll 2000 hep-th0011110
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Cl
Radiation dominated
Matter dominated
recombination
Large scales
Small scales
Lineweaver 1997
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Opaque Electrons
Boomerang
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Radiation domination
Matter domination
fertilization
CDM growing
baryons growing
equality
CDM growing
baryons growing
n
g
photon-baryon fluid
oscillating
oscillating
separation
Silk damping
Efstathiou 1990
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Cl
Radiation dominated
Matter dominated
recombination
Large scales
Small scales
Lineweaver 1997
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Quadrupole
Quadrupole l2
Lineweaver 1997
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NormalizationdT or As or Q10
CMB MoviesStarring CMBFASTDirected by Max
Tegmark
dT 60 mK
dT 30 mK
dT 0 mK
www.hep.upenn.edu/max/cmb
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CMB Movies dm and neutrinos
all dm neutrinos
no neutrinos
bm dominated
dm dominated
0.15 lt Wdh2 lt0.001
0.01 lt Wbh2 lt 0.15
0 lt fn lt 1
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Closed Open
L Dominated
Matter Dominated
-1.1 lt Wk lt 0.3
0 lt WL lt 0.9
0.3 lt h lt 1.3
0.4 lt h lt 1.2
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Bump growth
1/3 dT/T
dr/r
b drg/rg
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t early reionization
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Geometry of the Universe
Positively Curved?
Flat?
Negatively Curved?
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Wm - WL plane
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Three Candidates
Mr Open
Mr Flat
Mr Closed
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Dark energy is just possibly the most
important problem in all of physics M.S. Turner
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n
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SN Ia
Tonry etal 0105413
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1997
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Identification of 2/3 of the Universe
Lineweaver 1998
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Wm, WL and H
WL
80
70
60
50
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Wm
Lineweaver 1999
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5 Sources
Combined
Wm
Wm
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Combining Results
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Constraints in Wm-WL plane
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The other two dont work