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Modern State of Cosmology

Cherenkov Conference- 2004. Modern State of Cosmology. V . N . Lukash Astro Space Centre of Lebedev Physics Institute. Observational status Structure formations Initial conditions Cosmological parameters Degeneracies   h   cb , n S  ,  8 Minimal model and its extensions

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Modern State of Cosmology

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

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

  3. Cosmic Hubble parameter Tegmarket al., 2003

  4. Observational status 0.02

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

  6. LSSandCMB scales , z < zeq: LSS : DM Keq-1 CMB : B  x Krec-1

  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. fc , fb , fFU (late)  m X  Model IU (early)AS nSS AT nT LSS spectrum CMB spectrum  IU FU + ( T ) IU FU

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

  12.  104k Tegmark, Zaldarriaga, 2002

  13. 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 ~ kH~ 1 mm-1 • Stretching inhomogeneities on cosmological scales by inflation, k >> kH~ 1100 Мpc-1

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

  17. Observational constraints on inflationary models

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

  19. Models and observational quantities (T/S - nS)

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

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

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

  23. Minimal model 4 parametersof MM: (error bars <10%)

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

  25. 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)

  26. Arguments for >0 • Hubble diagram: SN Ia (correction for metallicity?) • Dynamics: ISW (galaxiesatz~0.5) • Structure: P(k)

  27. Reiss et al., 2002

  28. Riess et al., 2004

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

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

  31. Structure argument (solid!) Keq=aH~mh2 =mh(h/Mpc)   CMB LSS

  32. ... 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

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

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

  35. Among best-fit models(WMAP & 2dF) m=1, =0 =0.2, c=0.7 H0= 45 km s-1 Mpc-1 ↓ contradiction: • local H0 (6070 km s-1 Mpc-1) (SZ, gravitational lenses: 50  20) • SN Ia • cluster evolution • Ly

  36. Degeneracies in cosmological parameter space (reason – bad data, region – 10 % of ММ): geometrical (mh2 ~ const, 0) tensor (nS ~ fb ) neutrino (m ~ f)

  37. Geometrical degeneracy(0=1.010.02) h05 = 0.7 T0 = 13.5 05/2 Gyrs

  38. Hubble constant and the age of the Universe vs tot Tegmarket al., 2003

  39. Tegmarket al., 2003

  40. 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 byCMB)  + af = b (m+  = 1,a = cb , b = 1 - cb)

  41. + 0.5f = 0.65  0.1 Arhipova et al., 2002

  42. Novosyadlyj et al., 2000

  43. Cosmological parametersCMB  LSS

  44. Conclusions

  45. Breaking degeneracy between initial and boundary conditions in cosmology Stable prediction: nS 1,   0,   0.60.7 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

  46. ??? 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

  47. 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 andLSS scales (relation between baryon asymmetryand dark matter) • T/S → energy scale of inflation

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