1. Modern State of Cosmology V.N. Lukash Astro Space Centre of Lebedev Physics Institute Cherenkov Conference-2004

2. Observational status Structure formations Initial conditions Cosmological parameters Degeneracies   h   cb, n S ,  8 Minimal model and its extensions Problems

3. Cosmic Hubble parameter Tegmark et al., 2003

4. Observational status 0.02

5. Coincidence between two scales: LSS (DM) and CMB (DB)

6. LSS and CMB scales z < z eq : K eq -1 DM K rec -1 B  x, LSS : CMB :

7. Message from the early Universe: Baryon asymmetry is related to dark matter

8. Independent determination of initial and boundary conditions

9. Theory of gravitational instability Zero order (Hubble diagram) First order (density perturbations spectrum) Cosmological model – in two functions

10. f c, f b, f FU (late)      m  X  Model IU (early)A S n S  S A T n T LSS spectrum  CMB spectrum  IUFU IUFU + ( T )

11. Data mapping in k-space data point : window spectrum  probability distribution in k space CMB : P (k)

12.  10 4 k Tegmark, Zaldarriaga, 2002

14. Cosmological initial conditions

15. 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 ~ k H ~ 1 mm -1 Stretching inhomogeneities on cosmological scales by inflation, k >> k H ~ 1  100 Мpc -1

17. Lagrangian theory of q field ( V.N.L., 1980): In conformal coordinates:

19. Observational constraints on inflationary models

20. V(  ): classification of potentials Large field inflation Small field inflation  (hybrid)-inflation

21. Models and observational quantities (T/S - n S )

22.  -inflation (  =4) Е.V.Mikheeva, V.N.Lukash, 2004

23. M.Tegmark et al., 2003 V(  )~1-(  /  * ) 2 0.9 0.6 0.3 WMAP + SDSS r = -8n T T/S = 0.6 r

24. Chaotic inflation: m  2 - solid grounds  4 - severe trouble If n S >1 -  -inflation n S <1 - «chaotic» or «new» or … Inflationary model will be recognized in the nearest future

25. Minimal model n S =1  0 =1  T/S=0  f =0  degeneracies:geometrytensorneutrino 4 parameters of MM: (error bars <10%)

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

27. 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)

28. Arguments for  >0 Hubble diagram: SN Ia (correction for metallicity?) Dynamics: ISW (galaxies at z~0.5) Structure: P(k)

29. Reiss et al., 2002

30. Riess et al., 2004

32. N.Kardashev, ApJ 150, L135 (1967)

33. Dynamical impact of vacuum cross-correlation between maps of galaxies and CMB

34. K eq = a H~  m h 2 =  m h (h/Mpc) Structure argument (solid!)  CMB  LSS

35. ... 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

36. Myers et al., 2003 Angular cross-correlation between distant QSOs and nearby clusters of galaxies (APM/SDSS)

37. Substructure in galaxy halo (simulations) Diemand et al., 2004  ~r -   (1, 3/2)

38. Among best-fit models (WMAP & 2dF)  m =1,   =0  =0.2,  c =0.7 H 0 = 45 km s -1 Mpc -1 ↓ contradiction: local H 0 (60  70 km s -1 Mpc -1 ) (SZ, gravitational lenses: 50  20) SN Ia cluster evolution Ly 

39. Degeneracies in cosmological parameter space (reason – bad data, region – 10 % of ММ): geometrical (  m h 2 ~ const,  0 ) tensor (n S ~ f b ) neutrino (  m ~ f )

40. Geometrical degeneracy (  0 =1.01  0.02) h  0 5 = 0.7 T 0 = 13.5  0 5/2 Gyrs

41. Hubble constant and the age of the Universe vs  tot Tegmark et al., 2003

43. If m <0.7 eV, then z <z rec (3T  m : z  10 3 [m /0.7 eV])  h 2 =  m /93 eV < 0.02   b h 2 f   /  m 0.1) CMB ⇒  cb h 2  m =  cb + ,  m (1- f )=const   cb (fixed by CMB)   + a f = b (  m +   = 1, a =  cb, b = 1 -  cb )

44.   + 0.5 f = 0.65  0.1 Arhipova et al., 2002

45. Novosyadlyj et al., 2000

46. Cosmological parameters CMB  LSS no GW, +GW, no +GW,,BBN mh2mh2 0.140.120.16 mhmh0.20.170.25 bh2bh2 0.0210.0250.020 fbfb 0.150.220.10 f --0.05 nSnS 1.01.1 T/S-0.20.3  000  0.70.80.6

47. Conclusions

48. Breaking degeneracy between initial and boundary conditions in cosmology Stable prediction: n S  1,    0,    0.6  0.7 Best-fit model: f ~ f b ~ 10%,  m ~ 0.4, h ~ 0.65 (MM: f b ~ 15%,  m ~ 0.3, h~ 0.7) If  m  0.3, then   0, h  0.7  m > 0.3,   0.1, h < 0.7

49. ??? m  0.04  0.4 eV (f <0.1: m <0.4 eV) early ionization (z~20) T/S  0.2 small C 2, C 3 distortions ~30, 200 high  2 the running parameter

50. Unsolved fundamental problems: Dark matter (multicomponent):  b  ,  c ~  m ~   Cosmological constant:   ~M 4 = (10 -3 eV) 4 = standard model: M ~1 TeV GUT: M ~10 13 GeV quantum gravity: M ~10 19 GeV Coincidence of СМВ and LSS scales (relation between baryon asymmetry and dark matter) T/S → energy scale of inflation

51. 2dF Galaxy Redshift Survey O.Lahav et al., 2002

52. Beyond concordance model:  opt ~ 0.17 Low C 2,3, 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)

53. T.Shanks, astro-ph/0401409 Cross-correlation between WMAP (94 GHz) and galaxy clusters (АСО, R  2)

54. T.Shanks, astro-ph/0401409