Quantum Origin of the Universe Structure

V MukhanovV. MukhanovASC, LMU, München, ,

Blaise Pascal Chair, ENS, Paris

Before 1990Before 1990

The Universe expandsp

Hubble lawHubble law

r v =Hrv t : r = 1 : 13,7bil. yearsr v

t :

v H: 13,7bil. years

There exists background radiation with the temperature T ≈ 3K

Penzias Wilson 1965Penzias, Wilson 1965

There is baryonic matter:4about 25% of 4He, D....heavy elements

Dark Matter???? baryonic origin???Dark Matter???? baryonic origin???

Large Scale Structure: clusters of galaxies!Filaments, Voids??????????????????????

After 90 - presentAfter 90 present

COBE 1992

2.725K BlackbodySpectrum of the CMBCMB

2009 l k2009 Planck

??????End 2012

Ground-based:ABS, ACBAR, ACT, AMI, APEX, APEX-SZ, ATCA, , , , , ,BICEP, BICEP2, BIMA, CAPMAP, CAT, CBI, Clover,COSMOSOMAS, DASI, FOCUS, GUBBINS, Keck Array,MAT, OCRA, OVRO, POLARBEAR, QUaD, QUBIC, QUIET,RGWBT, Sakaatoon, SPT, TOCO, SZA, Tenerife, VSA

Expanding Universe: Facts The Universe is homogeneous and Today:

isotropic on scales from 300 millions 13 billi li hup to 13 billions light-years

There exist structure on small scales:There exist structure on small scales:Planets, Stars, Galaxies, Clusters of galaxiesa ets, Sta s, Ga a es, C uste s o ga a esSuperclusters ....

There is nd 75% , 25% aH He∼ ∼heavy elements in very small amounts

In past the Universe was VERY hot

Th i t D k M tt d D k E

p

There exist Dark Matter and Dark Energy

When the Universe was about 1000 times smaller, it was extremely homogeneous

δε 5and isotropic in scales l 10a l δεε

−∼

a

1aλ ∝

1Ta

∝a

When the Universe was 1000 times smallerWhen the Universe was 1000 times smallerits temperature was about 2725 K°

RecombinationNucleosynthesis RecombinationNucleosynthesis

??????Neutrinos decoupling,Electron-Positron pairs

ihil ti ( 1 k)

Quark-gluon phase transition

annihilation ( 1 sek)-4 10 sec1010 t −∼

∼ ∼

Electro-weak phase transitionp

V h I hVery homogeneous Inhomogeneous

INFLATIONINFLATION

INFLATION i th t f l t dINFLATION is the stage of acceleratedexpansion in the very early Universep y y

a&

decelerated Friedmann Expansiondecelerated Friedmann Expansion

0a&a&

INFLATION

t0titia

ic t

ΩE 0

pot

11000000009Ω 0 ≡0

E 0kin 1= 1000000003 =

Ekin = 3 +1000000000

PredictionEpot =−9 −1000000000

Predictionof inflation !

How gravity can become "repulsive"?4 Ga aπ ε= −&& ( )3p aε+3 ( )3p aε+acceleration energydensity pressure

" ti it "+3 0 0O l if && "antigravity"+3 0 0 Only if p aε < > ≡⇒

Scenarios???????????????????????????????????????????

Energy density pressure , pε

( )( ) equation of s etatp ε −f i fl ifor inflationp ε ε+ «

hi h i li dp ε≈ −

Which concrete scenario was realized ???

Quantum Fluctuations and Galaxies

Inflation "wash out" all existing classical inhomogeneities and leaves classical desert

Where the ihhomogeneities come from?

p x hΔ Δ ≥

There always exist unavoidable Quantum Fluctuations

Quantum fluctuations in the density distribution are large (10-5 )Q y g ( )only in extremely small scales ( : 10-33 cm),

58 25 but very small ( : 10

-58 ) on galactic scales ( : 1025 cm)Can we transfer the large fluctuations from extremely small scales to large scales???

!!!Yes only if in past the Universe went throughbut!!!Yes only if in past the Universe went throughthe stage of accelerated expansion (inflatbut

ion)

PREDICTIONSPREDICTIONS

Perturbations are :Perturbations are :-adiabaticadiabatic-gaussian: Φ=Φg + fNLΦg

2 , where fNL = O(1)g g fNL g , fNL ( )

-spectrum: Φ ∝ ln (λ /λγ ) ∝ λ1−nS with nS = 0.96p ( γ ) S

with Ωtot = 1 (prediction) and H0 , ΩΛ ,Ωbar from supernova, deuterium et.cet. we gettot (p ) 0, Λ , bar p , g

Planck FrequencyMaps

−Ωtot = 1± 0.0066−adiabatic pert.!!!, less than 1% from cosmic strings, entropy et.cet.−gaussian: fNL = 2.5 ± 5.8−nS =0.9585 ± 0.0070

CONCLUSIONS

General Relativity is valid up to the scales 10−27 cm−General Relativity is valid up to the scales 10 7 cm−We all originated from quantum fluctuationsg q