the perturbed universe: 1. cosmic microwave background...cosmic microwave background! feb 2011!...
TRANSCRIPT
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1!
Hervé Dole !Institut d’Astrophysique Spatiale, Orsay!Université Paris Sud 11 & CNRS & IUF!http://www.ias.u-psud.fr/dole/m2.php!
Montage: CMB, LSS, galaxies: SPACE!
the perturbed universe:"1. cosmic microwave
background!
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I. Angular Power Spectrum on the sphere: C_l!
1. What is a power spectrum ?!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 2!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 3!
Fourier analysis!C
ourt
esy
Mar
c-A
ntoi
ne M
iville
-Des
chên
es!
Espace direct: temps!
Espace conjugué: fréquence temporelle!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 4!
Cou
rtes
y M
arc-
Ant
oine
Miv
ille-D
esch
ênes!
1 sinus!centré!
2 sinus!centrés!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 5!
Cou
rtes
y M
arc-
Ant
oine
Miv
ille-D
esch
ênes!
n sinus!décentrés!
n sinus!centrés!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 6!
Cou
rtes
y M
arc-
Ant
oine
Miv
ille-D
esch
ênes!
n sinus!décentrés!
Forme!autosimilaire!
(fractale)!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 7!
Cou
rtes
y M
arc-
Ant
oine
Miv
ille-D
esch
ênes!
n sinus!décentrés!
WMAP 1 yr!
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I. Angular Power Spectrum on the sphere: C_l!
3. What is l (ell) ?!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 8!
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multipoles applied to the CMB!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 9!
Hinshaw et al., 2007, WMAP3!
Ylm courtesy Benoit Mosser, LESIA!
l=2!
l=3!
l=4!
l=5!
l=6!
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II. Observations of the Cosmic Microwave Background!
1. Measurements!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 10!
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Cosmic Microwave Background!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11!
Découvert en 1965 par !Arno Penzias & Robert Wilson.!
Nobel Prize 1978 "for their discovery of the !cosmic microwave background radiation" !
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properties!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 12!
Blackbody Radiation!T=2.725 K!
L’Univers est rempli de rayonnement: la nuit n’est pas noire, mais brillante en radio.!
Nobel Prize 2006: John Mather, GSFC!(1989 measurements)!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 13!
CMB by COBE in 1992!
Nobel Prize 2006: G. Smoot, GSFC!(1992 measurements)!
«#for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation#»!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 14!
fluctuations de température!
WMAP Web Site!
l’amplitude des fluctuations est de l’ordre de la dizaine de microKelvin ! !
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 15!
fluctuations de température!
WMAP Web Site!
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fluctuations de température!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 16!
WMAP 7 year!
WMAP Web Site!
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fluctuations de température!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 17!
Planck 1 an!
Planck ESA HFI LFI consortia!
+ Galaxie et galaxies, amas etc.!
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II. Observations of the Cosmic Microwave Background!
2. Strategy and Difficulties!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 18!
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you play !!
! we give you 600 ME to accurately measure the CMB!! its temperature and polarization anisotropies!
! what telescope and instrument would you build ?!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 19!
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CMB observations!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 20!
2009
Even Better !
1999 MAXIMA
1999 Boomerang
2000 Archeops
Planck (ESA) (Simulated)
WMAP web site & H. Dole!
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difficulties!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 21!
http://arcade.gsfc.nasa.gov/science_galaxy.html!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 22!
Détecteur
Poussière
Synchrotron
Free Free
Galaxies
SZ-thermique
SZ-cinetique
!T/T La poussière domine à hautes
fréquences et est donc un avant-plan important pour les observations bolométriques!
143 217 353 545 GHz
Courtesy N. Ponthieu, IAS!
Bou
chet
& G
ispe
rt!
«#Sandwich Cosmique#»!
foregrounds!
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foregrounds!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 23!
Courtesy N. Ponthieu, IAS!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 24!24!
"!
Grain!
B
Polarisation de l'émission thermique de la poussière!
• These grains align with the Galactic magnetic field and have selective absorption in the visible and UV…!
• … which in turn leads to selective radiation in the submm!
Optical polarization!
submm polarization!#!
+ Manque de mesures à grandes échelles!
(Stein 66)!
Serkowski et al 75!Heiles 01!Fosalba et al 02!
Courtesy N. Ponthieu, IAS!
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II. Observations of the Cosmic Microwave Background!
3. Description of the Angular Power Spectrum!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 25!
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TT angular power spectrum: 3 regimes!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 26!
1. Plateau!
2. Acoustic Peaks![Pics acoustiques]!
3. Damping![amortissement]!
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TT angular power spectrum: 3 regimes!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 27!
1. Plateau! 3. Damping![amortissement]!
2. Acoustic Peaks![Pics acoustiques]!
> horizon! subhorizon!
Hor
izon
@ r
ecom
b!
Thic
knes
s La
st S
c. S
urf.!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 28!
angle and geometrie!
Hu, Sugiyama, Silk, 1999!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 29!
angular distance!
Hu & Dodelson, 2002, ARAA! WMAP
@z~1100
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WMAP 5 TT !
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 31!
Dunkley et al., 2008, WMAP5!
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TT power spectrum at high ell!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 32!
Shirokoff et al., 2010!
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polarized microwave sky!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 33!
WMAP 3!
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TT & TE!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 34!
Jarosik et al., 2009, WMAP7!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 35!
TT
TE
EE
BB
lensing
Synchrotron+dust
Page et al., 2007, WMAP3!
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II. Observations of the Cosmic Microwave Background!
4. C_l and Cosmological Parameters!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 36!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 37!
origine of fluctuations!
Matière => puits de potentiel
Puits de potentiel - les photons qui tombent se réchauffent
(compression) - les photons qui en sortent sont refroidis
(détente)
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 38!
acoustic waves at recombination!
La physique de ces ondes dépend des paramètres cosmologiques
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C_l!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 39!
Hu & Dodelson, ARAA, 2002!
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II. Observations of the Cosmic Microwave Background!
5. Polarization!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 40!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 41!
CMB polarization for dummies!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 42!
Diffusion Thomson : d$/d% ~ |&.&’|2
& x
y
z
e- &’
Rayonnement isotrope (monopole)!
avec !T~1/m2 -> e- et d": angle solide
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 43!
Diffusion Thomson : d$/d% ~ |&.&’|2
& x
y
z
e- &’
Rayonnement isotrope (monopole)!
x’ = z y’ = y
z’
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 44!
Diffusion Thomson : d$/d% ~ |&.&’|2
& x
y
z
e- &’
Rayonnement isotrope (monopole)!
x’ = z y’ = y
z’
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 45!
Diffusion Thomson : d$/d% ~ |&.&’|2
& x
y
z
e- &’ x’ = z
y’ = y
z’
Rayonnement isotrope (monopole)!
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 46!
Diffusion Thomson : d$/d% ~ |&.&’|2
& x
y
z
e- &’ x’ = z
y’ = y
z’
Pas de polarisation!
Rayonnement isotrope (monopole)!
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 47!
& x
y
z
e-
Dipole!
&’ x’ y’
z’
Pas de polarisation!
Diffusion Thomson : d$/d% ~ |&.&’|2
Courtesy N. Ponthieu, IAS!
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Recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 48!
& x
y
z
e-
Quadrupole!
&’ x’ y’
z’
Polarization !
Diffusion Thomson : d$/d% ~ |&.&’|2
Courtesy N. Ponthieu, IAS!
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quadrupoles at recombination!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 49!
Les sur (sous) densités génèrent de la polarisation (vitesse)!
On sonde directement la recombinaison!
Rees, 1968!
Courtesy N. Ponthieu, IAS!
Over (under) densities generate polarization (speed)!
Polarization: a direct probe of recombination processes!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 50!
surdensité sousdensité Perturbations scalaires
Perturbations tensorielles
La polarisation permet de distinguer les différents types
de perturbation
Parité
Parité
x
y
Première possibilité de détection des ondes gravitationnelles primordiales générées pendant la phase d’inflation
Courtesy N. Ponthieu, IAS
«!modes E!»
«!modes B!»
![Page 51: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/51.jpg)
polarization data !!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 51!
WMAP7 Komatsu et al., 2009!
Planck data (embargoed) really!look like the simulations !!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 52!
" Il faut une anisotropie quadrupolaire pour générer de la polarisation!
" Les fluctuations de densité (scalaires) et les ondes gravitationnelles (tensorielles) créent des quadrupoles!
" Les figures de polarisation sont différentes!
Spectre de puissance et physique…!
Courtesy N. Ponthieu, IAS
polarisation: bilan!
![Page 53: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/53.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 53!
'x
y
Q = Ix - Iy
'x
y
U = Ix45 - Iy45
I, Q, U donnent une description complète de l’etat de
polarisation!
I = Ix + Iy
Courtesy N. Ponthieu, IAS!
les paramètres de Stokes!
![Page 54: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/54.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 54!
TT, EE, TE: behaviour!
Balbi et al., 2006!
TT
EE
TE
phase shift: opposition![déphasage: opposition
de phase]!
phase shift: half![déphasage de pi/2]!
![Page 55: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/55.jpg)
4 CMB anisotropies power spectra!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 55!
TB, EB = 0!B : pseudo-scalaire!
T, E : scalaire!
OK
OK
OK
KO ?
Courtesy N. Ponthieu, IAS!
3 observables: T, E, B!
![Page 56: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/56.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 56!
why polarization helps!
TT
EE & BB
Seules des observations en polarisation peuvent discriminer entre le «#CDM standard#» et le «#CDM + energie noire + ondes gravitat ionnel les + reionisation#»!
Balbi et al., 2006!
![Page 57: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/57.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 57!
anisotropies secondaires!
2ème diffusion Thomson lors de la
Réionisation!
Distorsion par effet de lentilles faibles!
Dark Energy + Neutrinos + Large Scale Structures!Courtesy N. Ponthieu, IAS!
B ( 0
B = 0
![Page 58: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/58.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 58!
qques résultats WMAP5!
Komatsu et al., 2008, WMAP5!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 59!
polarisation et spectre de puissance!W
ayne H
u,
Chic
ago:
htt
p:/
/bac
kgro
und.u
chic
ago.
edu/~
whu/i
nte
rmedia
te/i
nte
rmedia
te.h
tml
![Page 60: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/60.jpg)
create your own CMB !!
! with CMBeasy: http://www.cmbeasy.org!! based on CMBfast!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 60!
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II. Observations of the Cosmic Microwave Background!
6. Degeneracies!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 61!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 62!
1. Dégénérescence «#essentielle#»!
(MCMC with WMAP) %tot = 1 ’’fixes’’ Ho and ) (cf. WMAP)
From CMB physics % h2, H0, )*
Courtesy M. Douspis, IAS
![Page 63: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/63.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 63!
1. Dégénérescence «#essentielle#»!
Blanchard, Douspis et al. 03,05 Tocchini, Douspis, Silk 04
From CMB physics Initial conditions versus Evolution
)=0.0
Courtesy M. Douspis, IAS
![Page 64: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/64.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 64!
2. Dégénérescence «#intégrale#»!
Douspis, Aghanim & Langer 06
From additional physics Secondaries and Foregrounds
Courtesy M. Douspis, IAS
![Page 65: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/65.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 65!
2. Dégénérescence «#intégrale#»!
Spergel et al., 2007, WMAP3
#: Profondeur optique
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 66!
2. Dégénérescence «#intégrale#»!
Spergel et al., 2007, in press WMAP3
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 67!
3. Dégénérescence «instrumentale»!
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II. Observations of the Cosmic Microwave Background!
7. Origin of fluctuations!
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 68!
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 69!
origine des fluctuations!
Matière => puits de potentiel
Puits de potentiel - les photons qui tombent se réchauffent
(compression) - les photons qui en sortent sont refroidis
(détente)
![Page 70: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/70.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 70!
Ondes Acoustiques à la Recomb.!
La physique de ces ondes dépend des paramètres cosmologiques
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 71!
Courbure!
Position du 1er pic acoustique <=> courbure de l’Univers Way
ne H
u,
Chic
ago:
htt
p:/
/bac
kgro
und.u
chic
ago.
edu/~
whu/i
nte
rmedia
te/i
nte
rmedia
te.h
tml
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 72!
Contenu en Baryons!W
ayne H
u,
Chic
ago:
htt
p:/
/bac
kgro
und.u
chic
ago.
edu/~
whu/i
nte
rmedia
te/i
nte
rmedia
te.h
tml
Position du 2nd pic acoustique <=> contenu en baryons
![Page 73: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/73.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 73!
Matière Noire!W
ayne H
u,
Chic
ago:
htt
p:/
/bac
kgro
und.u
chic
ago.
edu/~
whu/i
nte
rmedia
te/i
nte
rmedia
te.h
tml
Position du 3ème pic acoustique <=> contenu en matière noire
![Page 74: the perturbed universe: 1. cosmic microwave background...Cosmic Microwave Background! feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 11! Découvert en 1965 par ! Arno Penzias &](https://reader035.vdocuments.site/reader035/viewer/2022070110/6046b0bb4160eb0de450be25/html5/thumbnails/74.jpg)
feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 74!
Pics Acoustiques dans le Sp. P.!W
ayne H
u,
Chic
ago:
htt
p:/
/bac
kgro
und.u
chic
ago.
edu/~
whu/i
nte
rmedia
te/i
nte
rmedia
te.h
tml
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feb 2011! Hervé Dole, IAS - M2 NPAC - Cosmology! 75!
Cosmic Microwave Background!
WMAP 3 yr