Modern State of CosmologyModern State of Cosmology

VV..NN.. Lukash LukashAstro Space Centre of Astro Space Centre of

Lebedev Physics InstituteLebedev Physics Institute

Cherenkov Conference-2004

• Observational status• Structure formations• Initial conditions• Cosmological parameters• Degeneracies

h cb, nS

, 8

• Minimal model and its extensions• Problems

7.03.0

h3/1

m

bSn

7.0e8

Cosmic Hubble parameter

Tegmark et al., 2003

Observational status

0.02

Coincidence between two

scales:

LSS (DM) and CMB (DB)

LSS and CMB scales

z < zeq: 2~

1

1

za

3

1100

3200

z

z

rec

eq

2

eq

rec

eqeq

1k

recrecSrec

3

c

1k

Keq-1DM

Krec-1

B

x

,

LSS :

CMB :

13k

k

eq

rec

rec

eq

Message from the early Universe:

Baryon asymmetry is related to dark matter

Independent determination of initial and boundary conditions

Theory of gravitational instability

• Zero order(Hubble diagram)

• First order(density perturbations spectrum)

Cosmological model – in two functions

(t)a

)z,k(P

fc , fb , f FU (late) m X

Model IU (early) AS nS S AT nT

LSS spectrum

CMB spectrum k

dk)k(W)k(PС

)z,k(T)k(P)z,k(P 2IU FU

IU FU

+ ( T )

Data mapping in k-space

k

dk)k(Pd ii

data point :

k

dk)k(P)k(WС

window spectrum probability distribution in k space

CMB :

P(k)

104 k

Tegmark, Zaldarriaga, 2002

Tegmark, Zaldarriaga, 2002

Cosmological initial conditions

Generation of density perturbations in the very early Universe

• Seeds – quantum vacuum fluctuations of density (phonons)

• Parametric amplification of density perturbations in the expanding Universe – spontaneous creation of phonons,

k ~ kH ~ 1 mm-1

• Stretching inhomogeneities on cosmological scales by inflation,

k >> kH ~ 1100 Мpc-1

dxdxhdtdx,C2dtD21ds 222 aa

,BAh2

1 ,v;D1u i

aa HvAHvq

qdtH

aa

,G4 C2

a H

q

p 2

CC

p

2

3

H

H2

p2 2

2

Lagrangian theory of

q field (V.N.L., 1980):

In conformal coordinates:

,,

222 qqqL

a

0qq2H3q 2

2a

k

0qUq 2

qq a

aa

)(

)(UU

Observational constraints on inflationary models

V(): classification of potentials

)exp(~)(V

~)(V

:0V

Large field inflation

Small field inflation

(hybrid)-inflation

C

0 1V)(V

:0V

4c;4

1V)(V

:0)0(V,0V

2С

С0

Models and observational quantities (T/S - nS)

-inflation (=4)

Е.V.Mikheeva, V.N.Lukash, 2004

0,8 0,9 1,0 1,1 1,20,0

0,2

0,4

0,6

0,8

1,0

c=80

c=22

c=12

c=9

c=7

T/S

nS

M.Tegmark et al., 2003

V()~1-(/*)2

0.9

0.6

0.3

WMAP + SDSS r = -8nT T/S = 0.6 r

• Chaotic inflation:

m2 - solid grounds

4 - severe trouble

• If nS>1 - -inflation

nS<1 - «chaotic» or «new» or …

• Inflationary model will be recognized in

the nearest future

Minimal modelnS=1 0=1

T/S=0

f=0

degeneracies: geometry tensor neutrino

4 parameters of MM:(error bars <10%)

84.0

023.0

123.0

7.0

17.0

8

b

c

A large number of observational points (~ 2000) can be fitted by only four parameters of MM

Reionization puzzle

QSO end of reionization: z~10

Evolution of star formation: flat out to z~6

Most distant galaxy: z~10 QSO: z=6.41

Two reionization epochs ?z~20 (massive stars)

z~10 (normal stars, QSO)

Arguments for >0

• Hubble diagram: SN Ia (correction for metallicity?)

• Dynamics: ISW (galaxies at z~0.5)

• Structure: P(k)

z11

a

3.014.0

)2.0( 2

m

2

m

hm 2mm h

LSS CMB

Reiss et al., 2002

Riess et al., 2004

N.Kardashev, ApJ 150, L135 (1967)

Dynamical impact of vacuumcross-correlation between maps of galaxies and CMB

~~G4 m aa2 ,const

,-1а

m

m

4aa

4

3

2m2 Th

~H

Keq=aH~mh2=mh (h/Mpc)

,h~h

~H:eq22

m

2m22

a

a 2mh~

1

a

Structure argument(solid!)

CMB

LSS

... and counter-arguments

• Weak lensing (m~1)• Problems of CDM:

– absence of cusps in galaxy centres (stability of galaxy bars)

– absence of substructure in galaxy halos (stability of spiral pattern in galaxy disks)

– small number of low-massive galaxies– flat luminosity and correlation functions

of galaxies

Myers et al., 2003

Angular cross-correlation between distant QSOs

and nearby clusters of galaxies (APM/SDSS)

Substructure in galaxy halo(simulations)

Diemand et al., 2004

~r -

(1, 3/2)

Among best-fit models(WMAP & 2dF)

m=1, =0=0.2, c=0.7

H0= 45 km s-1 Mpc-1

↓contradiction:

• local H0 (6070 km s-1 Mpc-1)(SZ, gravitational lenses: 50 20)

• SN Ia• cluster evolution• Ly

Degeneracies in cosmological parameter space

(reason – bad data,

region – 10 % of ММ):

geometrical (mh2 ~ const, 0 )

tensor (nS ~ fb )

neutrino (m ~ f)

Geometrical degeneracy(0=1.010.02)

h05 = 0.7

T0 = 13.5 05/2 Gyrs

Hubble constant and the age of the Universe vs tot

Tegmark et al., 2003

Tegmark et al., 2003

If m<0.7 eV, then

• z<zrec (3T m: z 103 [m/0.7 eV])

h2 = m/93 eV < 0.02 bh2

• f / m < 0.2 (for mh2 > 0.1)

CMB ⇒ cbh2

m= cb+ , m(1- f)=const cb (fixed by CMB)

+ af = b

(m+ = 1, a = cb , b = 1 - cb)

+ 0.5 f = 0.65 0.1

Arhipova et al., 2002

73.0n m

66.0f7.0

Novosyadlyj et al., 2000

Cosmological parameters CMB LSS

no GW,

+GW, no +GW,,BBN

mh2 0.14 0.12 0.16

mh 0.2 0.17 0.25

bh2 0.021 0.025 0.020

fb 0.15 0.22 0.10

f - - 0.05

nS 1.0 1.1 1.1

T/S - 0.2 0.3

0 0 0

0.7 0.8 0.6

ConclusionsConclusions

• Breaking degeneracy between initial and boundary conditions in cosmology

• Stable prediction:

nS 1, 0, 0.60.7

• Best-fit model: f ~ fb ~ 10%, m ~ 0.4, h ~ 0.65

(MM: fb ~ 15%, m ~ 0.3, h~ 0.7)

• If m 0.3 , then 0, h 0.7

m > 0.3 , 0.1, h < 0.7

• ???

m 0.04 0.4 eV

(f<0.1: m <0.4 eV)

early ionization (z~20)

T/S 0.2

small C2, C3

distortions ~30, 200

high 2

the running parameter

Unsolved fundamental problems:

• Dark matter (multicomponent):

b , c~m~

• Cosmological constant: ~M4 = (10-3eV)4=

standard model: M ~1 TeV

GUT: M ~1013 GeV

quantum gravity: M ~1019 GeV

• Coincidence of СМВ and LSS scales

(relation between baryon asymmetry and dark matter)

• T/S → energy scale of inflation

2dF Galaxy Redshift Survey

O.Lahav et al., 2002

Beyond concordance model: opt ~ 0.17

• Low C2,3, deviations (>3) at l~30, 200

• Rolling of spectral index• Poor 2 of concordance model (others in 1)• Spectral excess at l~2500 (CBI, ACBAR)

QSO: end of reionization at z~6

Evolution of star formation: flat out to z~6

Most distant galaxy: z=6.56

QSO: z=6.41

New: two reionization epochs

At z~20 (massive stars, QSO)

At z~6 (normal stars, QSO)

T.Shanks, astro-ph/0401409

Cross-correlation between WMAP (94 GHz) and galaxy clusters (АСО, R2)

T.Shanks, astro-ph/0401409