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CMB as a physics laboratory. Recombination. T = 0.3 eV H -1 . - PowerPoint PPT Presentation
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CMB as a physics CMB as a physics laboratorylaboratory
RecombinatioRecombinationn
Hydrogen is neutralHydrogen is ionized
Thomson Scattering
T = 0.3 eV << me c2
CosmicCosmic
Tegmark, 2000
Dust
Point sources
Free freeSynchrot.
MicrowaveMicrowaveDecoupling: photon mean free path, ne
Tdec=3000K depends essentially only on the baryon density (ne) and on the total matter density (H-1 ).
After 10Gyr, this has to cool by a factor of roughly 1000: the present black body spectrum at Tcmb=2.726K is then an immediate indication that the values of totb H0 we currently use are in the right ballpark.
BackgroundBackground
CMBz = 1100
HistoryHistory19411941 McKellarMcKellar
CH,CN excitation CH,CN excitation
temperature in starstemperature in stars
19491949 GamowGamow
Prediction TcmbPrediction Tcmb
19641964 Penzias WilsonPenzias Wilson 1010-1-1
19661966 Sachs WolfeSachs Wolfe
DT/T grav.DT/T grav.
19701970 Peebles YuPeebles Yu
DT/T ThomsonDT/T Thomson
19921992 COBECOBE 1010-4-4 7700
19991999 BoomerangBoomerang 1010-5-5 2020’’
20022002 DASIDASI
PolarizationPolarization
20032003 WMapWMap 1010-5-5 1818’’
20072007 PlanckPlanck 1010-6-6 77’’
Is the Universe….Is the Universe….
Open, closed, flat, compact,Open, closed, flat, compact,
accelerated, deceleratedaccelerated, decelerated, ,
initially gaussian, scale invariant,initially gaussian, scale invariant,
adiabatic, isocurvature,adiabatic, isocurvature,
einsteinianeinsteinian…?…?
• GeometryGeometry• DynamicsDynamics• Initial conditionsInitial conditions• Growth of Growth of
fluctuationsfluctuations
Ask the CMB….Ask the CMB….
What do we expect to find What do we expect to find on the CMB?on the CMB?
• oo , ,bb ,n ,n R,NR R,NR ,H,H00
• nnss, n, nt t , ,
• inflation pot. V (inflation pot. V ()) ww· VEPVEP• topological defectstopological defects• bouncing universebouncing universe• Compact topologyCompact topology• Extra dimensionsExtra dimensions
the standard universe
the unexpected universe
the weird universe
XXXXXboring
XXXXXXXexciting
very exciting XXXX
Perturbing the CMBPerturbing the CMB• Observable: radiation intensity per unit frequency per Observable: radiation intensity per unit frequency per
polarization state at each point in sky:polarization state at each point in sky:
P, P, EE• In a homogeneous universe, the CMB is the same perfect In a homogeneous universe, the CMB is the same perfect
black-body in every directionblack-body in every direction
• In a inhomogenous universe, the CMB can vary in:In a inhomogenous universe, the CMB can vary in:
intensityintensity Grav. Pot, Doppler, intrinsic Grav. Pot, Doppler, intrinsic fluctuationsfluctuations
polarizatiopolarizationn
anisotropic scattering, anisotropic scattering, grav. wavesgrav. waves
PP
spectrumspectrum energy injection z<10energy injection z<1066 EE
Predicting the CMBPredicting the CMB
• General relativistic equations for baryons, dark General relativistic equations for baryons, dark matter, radiation, neutrinos,...matter, radiation, neutrinos,...
• Solve the perturbed, relativistic, coupled, Solve the perturbed, relativistic, coupled, Boltzmann equationBoltzmann equation
• Obtain the DT/T for all Fourier modes and at all Obtain the DT/T for all Fourier modes and at all timestimes
• Convert to the DT/T on a sphere at z=1100 Convert to the DT/T on a sphere at z=1100 around the observeraround the observer
Complicate but linear !
Fluctuation spectrumFluctuation spectrum
From DT/T To Cl
Largescales
Smallscales
Temperature fluctuationsTemperature fluctuations
ArchaicArchaic
(>horizon (>horizon scale)scale)
Middle AgeMiddle Age ContemporaryContemporary
(<damping (<damping scale)scale)
> 2> 200
l l < 100< 100 220 0 < < <10’ <10’
100 < 100 < l l < < 10001000
< 10’< 10’
l l > 1000> 1000
zz>>1000>>1000 1000>1000>zz>1>100
zz<10<10
Archaic CMBArchaic CMB
• Sachs-Wolfe effect of Sachs-Wolfe effect of superhorizonsuperhorizon inflationary perturbationsinflationary perturbations
• Integrated Sachs-Wolfe effect of Integrated Sachs-Wolfe effect of subhorizonsubhorizon fluctuations: when the fluctuations: when the gravitational potential is not constant gravitational potential is not constant (eg, nonflat metric, other components, (eg, nonflat metric, other components, non-linearity, etc)non-linearity, etc)
Sachs-Wolfe effectSachs-Wolfe effect
Last Scatt. Surface
ISW
SW
z = 1100
z = 0
.
Fluctuation spectrumFluctuation spectrum
22)(
),(),(
),(),(
expansionharmonicSpherical
mm
mm
mmm
T
TaC
dYT
Ta
YaT
T
Sachs-Wolfe effectSachs-Wolfe effect
Data: Cobe +Boomerang
P(k)=Akn
)1(4
)()(
ZeldovichHarrison
)()()(),(
:Spectrum
)()(2
3)()(4
:spacek in Poisson3
WolfeSach
40
2
22242
2222
AHC
AkakP
kjadkaHdkkGT
TC
aaaHaaak
T
T
s
SW
k
dkmok
SW
kmok
Integrated Sachs-Wolfe Integrated Sachs-Wolfe effecteffect
))()(()(
),(
:
22224
2
aaadt
dkdtjdkH
dtT
T
dt
dkGdkC
Spectrum
kmo
k
ISW
Middle age CMBMiddle age CMB
• Acoustic perturbations:Acoustic perturbations:• perturbations oscillate acoustically perturbations oscillate acoustically
when their size is smaller than the when their size is smaller than the soundsound horizonhorizon (the pressure wave (the pressure wave has the time to cross the has the time to cross the structure)structure)
• The oscillations are The oscillations are coherent !coherent !
The sound horizon at The sound horizon at decouplingdecoupling
•The decoupling occurred 300,000 yrs after the big bang•Acoustic perturbations in the photon-baryon plasma travelled at the sound speed
Therefore they propagated for
(almost) independently of cosmology.
3/ccs
Mpclyr 05.0000,170
Acoustic oscillationsAcoustic oscillations
LSS
z = 1100
z = 0
Coupled fluctuationsCoupled fluctuations
D. Eisenstein
Acoustic oscillationsAcoustic oscillations
First peak: Sound horizonFirst peak: Sound horizon
• angular size : sensitive to the angular size : sensitive to the dominantdominant components components
• amplitude : sensitive to the amplitude : sensitive to the baryonbaryon componentcomponent
Sound Sound horizonhorizon
SHSH
D
SHSH
zs
kk
kk
z
R
R
zE
dzcSH
kx
kx
kx
xS
zEHHzE
dzcSH
kr
drtadtc
dsFRW
d
d
deg1
)(r
horizon sound
1)sinh(
0
1)sin(
)(
)(,)(
r
distance1
)(
0
10SH
2/12/1
2/12/1
00
10D
2
2222
2
SH
DR
SHR
Acoustic peaksAcoustic peaks
Data: Boomerang 1999
Contemporary CMBContemporary CMB
• Processes along the line-of-sight:Processes along the line-of-sight:• SZ effect: inverse Compton SZ effect: inverse Compton
scattering (scattering (cluster massescluster masses))• stochastic lensing (stochastic lensing ( mass mass
fluctuation powerfluctuation power))• reionization (reionization ( epoch of first lightepoch of first light))
Temperature field Lensed temperature field
Weak Lensing in CMB
Hu 2002
How is polarization How is polarization generated? generated?
Thomson Scattering
GravityWaves
Density pert. &
Gravity Waves
CMBCMBin in 1999…1999…
……20012001
……20032003
SensitivitySensitivity Hu, 2002
Now
Map, 2003
Planck, 2007
The geometric effectThe geometric effect
The kinematic effectThe kinematic effect
)'(
')(
zH
dzzr