MYSTERIES IN THE SKY A.D. Dolgov. University of Knoxville November, 20, 2006

Transcription

1 MYSTERIES IN THE SKY A.D. Dolgov ITEP, , Moscow, Russia University of Ferrara 40100, Italy INFN, Ferrara 40100, Italy University of Knoxville November, 20,

2 FUNDAMENTAL DISCOVERIES OF THE XX CENTURY 1. Antigravitating dark energy, DE 2. New form of matter, DM. 3. Protons are not forever. 4. Inflation in cosmology (and in everyday life). Now about 100 pages to follow... 2

3 Let us make a few gedanken (thought) experiments. 1. Throw a stone up from the Earth surface. It would slow down and, depending upon the initial velocity, V, either return back, V < V 0, or disappear in cosmic space V > V 0, or come to a stationary orbit, V = V 0 (more precisely, V(r ) 0). 3

4 The same was believed to be true in cosmology. The universe expansion (it is the same inertial motion as that of the stone) should slow down, ä < 0 and the universe would either 1) collapse back, closed universe, 2) or she would expand forever (open universe), 3) or, intermediate case, eternal expansion with flat Euclidean geometry. 4

5 Astronomical data showed that this is not the case. Expansion is accelerating: ä a = 4π 3m 2 (ρ + 3p) > 0 P l antigravity in action! Here G 1 N m2 Pl = GeV. [System of units: c = k = h/(2π) = 1.] In fact, initially acceleration, then normal deceleration, and acceleration again today. 5

6 In General Relativity not only mass (energy) creates gravitational force but also pressure, ä (ρ + p). With Newtonian gravity our universe, including ourselves would not exist. Antigravity at the beginning was a source of expansion - inflation. But do we need it now? 6

7 Equation of state: p = wρ For antigravity p < ρ/3 is necessary. The data show that w 1. About 75% of the universe mass is made of this strange matter, dark energy. NB: if ρ > 0 antigravity exists only for infinitely large systems. No antigravitating space ships. 7

8 Comment: w = 1 corresponds to vacuum energy, i.e. T µν = ρ vac g µν The only invariant symmetric tensor of the second rang is the metric tensor g µν. It looks the same in all coordinate systems, i.e. vacuum. Terrible problems with vacuum energy! Maybe principle of relativity is broken? 8

9 If w < 1/3 even a closed universe will expand forever. Still nothing will happen with our galaxy, she only will become older and older. Other galaxies will disappear form the sky, but we do not see them without telescopes. What happens if w < 1 (phantom cosmology)? Everything will be torn apart, not only galaxies but also atoms and even elementary particles. Pathological theories, should be forbidden by law. 9

10 2. Look around: all are made of protons, neutrons, and electrons. We believed that this is the dominant form of matter in the universe, plus a minor fraction made of photons (CMBR, stellar light) and neutrinos. 10

11 Cosmology proves that this normal matter makes only 1/5 of the other unknown form of matter: Dark Matter. Together with baryonic matter they make 25% of the total mass of the universe. We are neither in the Center of the universe nor are made of the most common matter. Humiliating or just the opposite? Maybe because of that we are precious as other rare species? 11

12 3. In any experiment baryons are conserved. In old textbooks: we exist, ergo protons are stable Now the motto is opposite: we exist ergo protons are unstable Cosmology has proven that either proton decays or n n transformation exists. All matter will ultimately disappear. 12

13 4. INFLATION 1. Origin of expansion. Big bang is not bomb explosion into empty space. 2. Temperature of CMBR is the same over all the sky, while only 1 degree is causally connected. 3. Ω tot = Spectrum of perturbations, slightly distorted Harrison-Zeldovich one. INFLATION IS AN EXPERIMEN- TAL FACT. Baryons are not conserved. 13

14 COSMOLOGY PROVES THAT NEW PHYSICAL PHENOMENA DO EXIST. 14

15 Two other possible titles: COSMOLOGY AND PHYSICS BEYOND THE STANDARD MODEL or COSMOLOGY AND NEW PHYSICS 15

16 Presently there are two established models/theories which are in perfect or almost perfect agreement with experiment/observations: 1. Minimal standard model in particle physics (MSM) and 2. Standard cosmological model (SCM). They do not match each other. New physics is necessary. 16

17 MSM in particle physics: Matter inventory: 3 families of quarks and leptons, gluons, weak W and Z bosons, photon. Gauge interactions: SU(3) SU(2) U(1). Gravity lives separately. 17

18 Theoretical problems: 1. Hierarchy of fermion masses. Neutrino oscillations 2. Hierarchy of electroweak ( GeV) and gravitational scales (10 19 GeV). 3. Include gravity! On the other hand, perfect agreement with experiment! No single hint to deviation from MSM, except for cosmological data. 18

19 STANDARD COSMOLOGICAL MODEL Theoretical setting, simple and robust. 1. General Relativity. 2. Homogeneous, isotropic matter, in zeroth approximation. Perturbations in first order if they are small or numerical simulation, when δρ/ρ 1. 19

20 3. Knowledge of cosmic particle content and form of their interaction; sometimes, but not always, equation of state exists and is sufficient: p = f(ρ) with p and ρ being pressure and energy densities of matter. 20

21 With a few free parameters SCM very well describes astronomical data, at per cent accuracy. Never in doubt but always in error, L. Landau, is not true now! But new physics beyond MSM is surely demanded. 21

22 WHAT IS NEW PHYSICS? New objects and interactions. Breaking of established rules or conservation laws. New principles. WHAT ELSE? 22

23 NATURAL NEW PHYSICS Almost inevitable: 1. New fields or/and particles, a) stable or quasistable b) heavy or light, dark matter, cold or warm, and maybe dark energy. BH as DM are not excluded (thus no new fields) but DE demands something really new. 23

24 2. Broken of charges/quantum numbers: a) electric, (impossible? or at least nontrivial with hi D); but if m γ 0, the universe must be electrically charged. b) baryonic (practically certain) c) leptonic (expected) d) leptonic family (discovered!); e, µ, τ leptons and corresponding neutrinos, µ does not decay into eγ, but ν e ν µ. We must look for µ eγ. 24

25 Less probable but still expected: 3. Topological or non-topological solitons. 4. New types of interactions, especially new long range forces, modified gravity. 5. Higher dimensions? 25

26 UNNATURAL NEW PHYSICS: 1. Breaking of Lorentz-invariance. 2. Violation of CPT. 3. Spin-statistics relation. 4. Unitarity, coherence. 5. Energy conservation. 6. Causality, time-machine. 7. Breaking of least action principle, Hamilton and Lagrange dynamics. 8. Principle of relativity. 26

27 UNEXPECTED NEW PHYSICS anything which is not in the list above and will never be there a priori. 27

28 Why do we need such drastic (crazy!) ideas? Surely crazy enough. Answer 1: Just curiosity, interesting to test. Cosmology may be the best laboratory to discovery and study new physics. Answer 2: problem of vacuum/dark energy quite likely demands new and even possibly UNNATURAL physics. 28

29 BACK TO THE PAST (brief universe history) 1. Beginning, unknown. Maybe time did not exist? 2. Inflation. Surely existed, experimental fact. 3. Baryogenesis, also experimental fact. 4. Thermally equilibrium universe, adiabatically cooled down. Some phase transitions on the way, GUT, EW, QCD, with huge change of vacuum energy and possible formation of topological solitons. 29

30 Well known epochs: 5. Neutrino decoupling, T 1 MeV. 6. Big bang nucleosynthesis (BBN), T = MeV. One of the cornerstones of SCM. Still some clouds are seen. 7. Onset of structure formation at RD MD, z eq 10 4, T ev. 30

31 8. Hydrogen recombination, z 10 3, T 0.2 ev. Decoupling of CMBR. Infall of baryons into already evolved seeds of structures. 9. Reionization, at z = 10 20? Formation of first stars. 10. Present time, t U = Gyr. 31

32 Universe today 1. Expansion rate: H = 100 h km/sec/mpc, h = 0.73 ± Energy density: ρ = ρ c = h 2 g cm 3 = 10.5 h 2keV cm GeV 4. Definition: Ω j = ρ j /ρ c. 32

33 MATTER INVENTORY Total energy density: Ω tot = 1 ± 0.1 from position of first peak of CMBR and LSS. Usual baryonic matter: Ω B = ± from heights of CMBR peaks, BBN, onset of structure formation and small δt /T. 33

34 Total dark matter: Ω DM 0.22 ± 0.04 from galactic rotation curves, gravitational lensing, equilibrium of hot gas in rich galactic clusters, cluster evolution, LSS. The rest: Ω DE induces accelerated expansion; from dimming of hi-z supernovae, LSS, universe age. 34

35 Different pieces of data and their interpretation are independent. It diminishes probability of interpretation error. 35

36 3 No Big Bang SNe: Knop et al. (2003) CMB: Spergel et al. (2003) Clusters: Allen et al. (2002) 2 Supernovae 1 Ω Λ 0 CMB expands forever recollapses eventually Clusters closed 1 open flat Ω M 36

37 caption 37

38 What is dark matter? Three possible types determined by the fluctuation dissipation scale l d : 1. CDM, l d < l gal ; 2. WDM, l d l gal ; 3. HDM, l d > l gal. 38

39 Possible forms of dark (invisible) matter. Several (too many?) candidates. Cold dark matter (CDM): 1. LSP, m = TeV. 2. Axion, m = 10 5 ev. 3. Mirror world. May contain CDM and WDM. 4. Black holes. 5. Topological and non-topological solitons, wimpzillas, heavy leptons, quark nuggets, heavy QCD-bubbles,??? 39

40 Warm dark matter (WDM): Sterile neutrino m = kev, may come from mirror world. Hot dark matter (HDM): Usual neutrinos, must be subdominant. A strong upper bound on their mass: mνj < 1 ev. 40

41 It seems that we need now both CDM and WDM, or maybe just WDM. Public opinion pool at the end of 80s: how many hypothetical forms of DM will survive to 2000? Answers: from 10 to 1. Today we have even more. 41

42 DARK ENERGY, unknown form of matter inducing accelerated expansion. Equation of state: p = wρ with w 1. Vacuum energy or cosmological constant T µν (vac) = ρ vac g µν, and p = ρ. The problems of dark energy and vacuum energy must be closely related. 42

43 PROBLEM OF VACUUM ENERGY. R µν 1 2 g µνr Λ g µν = 8πG N T µν Λ is equivalent to vacuum energy density, L.h.s. or r.h.s.? T (vac) µν = ρ vac g µν, Λ = 8πρ vac /m 2 P l. 43

44 1. Theoretically: Λ. Mismatch between theory and data: ORDERS OF MAGNITUDE. 2. Majority point of view during long time and maybe even now: = 0 Corrections are infinite but small (R. Feynman). 44

45 3. New independent pieces of data: EMPTY SPACE (ANTI)GRAVITATES. Is it vacuum with nonvanishing energy density? 4. Close proximity of ρ vac = const to ρ c 1/t 2 exactly today. 5. If antigravitating substance is not vacuum energy then WHAT? 45

46 Biographical notes Name(s): Cosmological constant, Λ-term, vacuum energy or, maybe, dark energy. Date of birth: 1918 Father A. Einstein. An attempt to make static universe. But why: the universe was known to be finite in space and time (Olberts paradox and thermal death). 46

47 Einstein attitude to his baby: The biggest blunder of my life (after Hubble s discovery of cosmological expansion). Many times assumed dead, probably erroneously. Well alive today. Still not safe - many want to kill it. 47

48 SOME MORE QUOTATIONS: Lemaitre: greatest discovery, worth to make Einstein s name famous. Gamow: λ raises its nasty head again (after indications that quasars are accumulated near z = 2 in the 60s) 48

49 Covariant conservation: D µ ( R µ ν 1 2 gµ ν R ) 0 automatic in metric theories. Analogy to electrodynamics: µ F µν = 4πJ ν Owing to anti-symmetry of F µν, µ ν F µν 0 and the current MUST be conserved, µ J µ = 0. 49

50 Automatic conservation of r.h.s. Einstein equations: [ D µ T ν (m)µ ] /(8πm 2 P l ) + Λg µν = 0 Due to covariant conservation of energymomentum tensor: D µ T µ (m) ν = 0, and the condition (in metric theory): D µ g µ ν 0, the cosmological constant must be CONSTANT: Λ = const of 50

51 Models with Λ = Λ(t) are not innocent, new fields to respect energy conservation condition are necessary or serious modifications of the theory, e.g. non-metric theories. First attempts to make time-dependent Lambda, 1935 by Bronstein (Leningrad); strongly criticized by Landau. 51

52 Seminar on Problems of Measurability in Quantum Gravity and of Da th Anniversary of Matvey P. Bronshtein s birth September of 1 11/07/ :43 PM %caption

53 RISE AND FALL OF LAMBDA-TERM 1. Birth: Ω v Hubble discovery of expansion, earlier Friedman solution: Ω v Lemaitre, De Sitter, later Eddington: one of the most important discoveries in GR. 4. Still non-zero Lambda is not accepted by majority. 5. QSO accumulation near z=2 explained by Ω v 1. Later rejected. 53

54 6. From 60s to the end of the Millennium Lambda was identically zero. Only a few treated it seriously, starting from Zeldovich. 54

55 7. End of 90s: a) Universe age crisis. With H 70 km/sec/mpc the universe would be too young, t U < 10 Gyr, while stellar evolution and nuclear chronology demand t U 13 Gyr. 55

56 b) Ω m = 0.3, measured by several independent ways: mass-to-light ratio, gravitational lensing, galactic clusters evolution (number of clusters for different red-shifts z). On the other hand: inflation predicts Ω tot = 1. Spectrum of angular fluctuations of CMBR (position of the first peak) measures Ω tot = 1 ±

57 c) Dimming of high redshift supernovae. Cannot be explained by dust absorption because it was found that the effect is non-monotonic in z. At larger z dimming decreases. Indeed, ρ m 1/a 3, while ρ vac = const. Equilibration at z

58 d) LSS and CMBR well fit theory if Ω m = 0.3 and Ω v 0.7. Theory: gravitational instability, flat spectrum of primordial fluctuations, cold dark matter (non-interactive?). CONCLUSION: Ω v = 0.7 ρ vac GeV 4 Ω m =

59 EVOLUTION OF VACUUM(-LIKE) ENERGY DURING COSMIC HISTORY 1. At inflation ρ vac ρ now v and was DOMINANT. But it was not real vacuum energy but vacuum-like energy of almost constant scalar field inflaton. 2. At GUT p.t. (if such era existed) δρ vac GeV 4 3. At electro-weak p.t. δρ vac 10 8 GeV 4 59

60 4. At QCD p.t. δρ vac 10 2 GeV 4 The magnitude of vacuum energies of gluon and chiral condensates are known from experiment! QCD vacuum is not empty but filled with condensates of quarks and gluons with negative energy. 60

61 After inflation till almost the present epoch ρ vac was always sub-dominant ρ vac started to dominate energy density only recently at z

62 Situation became very grave after it was found that ρ vac 0 and today: [ρ vac = const] [ρ c 1/t 2 ]. 62

63 CONTRIBUTIONS TO VACUUM ENERGY 1. Bosonic vacuum fluctuations: d 3 k ω k H b vac = (2π) 3 2 a k a k + b k b k vac d 3 k = (2π) 3 ω k = 4 2. Fermionic vacuum fluctuations: d 3 k ω k H f vac = (2π) 3 2 a k a k b k b k vac d 3 k = (2π) 3 ω k = 4 Bosonic/fermionic cancellation - Zeldovich prior to SUSY. 63

64 Supersymmetry: N b = N f and m b = m f, then ρ vac = 0 if the symmetry is UNBROKEN. Soft SUSY breaking necessarily leads to ρ vac 10 8 GeV 4 0 Broken SUGRA allows for ρ vac = 0 but the natural value is ρ vac m 4 P l 1076 GeV 4 Phase transitions in the course of cosmological cooling δρ vac GeV 4 64

65 QCD is well established and experimentally verified science leads to conclusion that vacuum is not empty but filled with quark and gluon condensates: qq 0 G µν G µν 0 both having NEGATIVE vacuum energy ρ QCD vac ρ c 65

66 Vacuum condensate is destroyed by quarks and the proton mass is: m p = 2m u + m d ρ vac l 3 p m u m d 5 ev. Who adds the necessary donation to make the OBSERVED ρ vac > 0 and what kind of matter is it? 66

67 INTERMEDIATE SUMMARY 1. Known and huge contributions to ρ vac but unknown mechanism of their compensation down to (almost) zero. 2. Observed today ρ vac ρ c. WHY? 3. What is the nature of antigravitating matter? Consistent with w = 1, vacuum? Mostly only problems 2 and 3 are addressed: a) modification of gravity; b) new field (quintessence) leading to accelerated expansion. 67

68 Most probably all three problems are strongly coupled and can be solved only after adjustment of ρ vac down to ρ c is understood. 68

69 POSSIBLE SOLUTIONS 1. Subtraction constant. 2. Anthropic principle. 3. Infrared instability of massless fields (gravitons) in DS space-time. 4. Dynamical adjustment. 5. Drastic modification of existing theory - breaking of general covariance, Lorentz invariance, rejection of the Lagrange/Hamiltonian principle,...??? 69

70 Remember: we need to explain only one number or a function if w 1. 70

71 Dynamical adjustment, as axionic solution of strong CP problem. New field Φ (scalar of higher spin) coupled to gravity is necessary. 1) Vacuum energy condensate of Φ 2) ρ(φ) compensates original ρ vac. 3) Negative energy density of Φ. 71

72 Generic predictions: 1. Change exponential expansion to power law one. 2. Compensation of vacuum energy is not complete but only down to terms of the order of ρ c (t). 3. Non-compensated energy may have an unusual equation of state. Unfortunately, no realistic model found starting from 1982 but existence of dark energy was predicted in 1982 based on this idea. 72

73 EXAMPLES OF ADJUSTMENT 1. Non-minimally coupled scalar field (AD, 1982): φ + 3H φ + U (φ, R) = 0 with e.g. U = ξrφ 2 /2. Solutions are unstable if ξr < 0. 73

74 Asymptotically: φ t and DS turns into Friedman, but T µν (φ) Fg µν and the change of the regime is achieved due to weakening of gravitational coupling: G N 1/t 2 Such a rise of M Pl was recently suggested as a mechanism to explain hierarchy between EW and Planck. 74

75 2. Vector field V µ (AD, 1985): L = η [F µν F µν /4 + (V;µ) µ 2] ( ) +ξrm 2 ln 1 + V2 m 2 Unstable solution: and V t t + c/t T µν (V t ) g µν + vanishing terms Logarithmic variation of gravitational coupling with time. 75

76 3. Second rank tensor field S µν (AD, 1994): L 2 = η 1 S αβ;γ S αγ;β + η 2 S α β;α Sγβ ;γ + η 3 S α α;β Sγ;β γ Components S tt and isotropic part of S ij δ ij are unstable: ( 2 t + 3H t 6H 2 )S tt 2H 2 s jj = 0 ( 2 t + 3H t 6H 2 )s tj = 0 ( 2 t + 3H t 2H 2 )s ij 2H 2 δ ij S tt = 0 where s tj = S tj /a(t) and s ij = S ij /a 2 (t). 76

77 Ill-defined theory with non-physical components, T tt and/or T ii becoming physical? Ogievetsky and Polubarinov: Photon and Notoph - gauge theory of scalar field described by t-component of vector V µ. 77

78 In all the cases after some period of exponential expansion DS is changed into Friedman and the dominant term in T µν g µν but G N is time-dependent. More important: in all the models above expansion rate is not related to the usual matter. 78

79 4. Scalar with crazy coupling to gravity (Mukohayama, Randall, 2003; AD, Kawasaki, 2003:) A = d 4 x [ g 1 2 (R + 2Λ) + F 1(R) Solution tends to + D µφd µ φ 2 R 2 U(φ, R) R ρ vac + U(φ) = 0 It has some nice features ( almost realistic ), H = 1/2t, etc but unstable with respect to small fluctuations. ] 79

80 Equation of motion for Φ: ( ) ] D µ [D µ 1 2 φ + U (φ) = 0. R GR equations for the trace, with F 1 = C 1 R 2 : ( ) 1 2 R + 3 (D α φ) 2 4 [U(φ) + ρ vac ] R ( ) 6D [2C (Dα φ) 2 ] 1 R = T µ µ R R 80

81 A desperate attempt to improve the model: (Dφ) 2 (Dφ)2 R R. R 2 81

82 More general action with scalar field (AD, Kawasaki, 2003) not yet explored: A = d 4 x g[ m 2 Pl (R + 2Λ)/16π +F 1 (R) + F 2 (φ, R)D µ φd µ φ +F 3 (φ, R)D µ φd µ R U(φ, R)] Moreover R µν and R µναβ can be also included. 82

83 INFLATION Period of exponential (or more generally accelerated) expansion in the early universe, a(t) exp [Ht] with H const. Energy-momentum tensor is vacuum like: T µν g µν Hence p = ρ and expansion is accelerated, ä/a (ρ + 3p) > 0. 83

84 We cannot live without inflation. 1. It solves the problems of homogeneity, isotropy, horizon, flatness. 2. Explains the origin of expansion - antigravitating state of matter before big bang. 3. Creates small initial density perturbations at astronomically large scales. 4. Creates all the matter out of microscopically small piece: dρ/dt (ρ + p) = 0. 84

85 INFLATION PREDICTS: 1. Geometrically flat universe, Ω = 1 ± Almost flat spectrum of perturbations with specific deviations. 3. Adiabatic Gaussian perturbations. All above are are observed. 4. Important to find gravitational waves from inflation. 85

86 Inflation is the only known way to create the observed universe, but be aware of weakness of no-go theorems in physics. Still inflation very much looks as an EXPERIMENTAL FACT INFLATION DEMANDS NEW FIELD, INFLATON absent in MSM. 86

87 END OF INFLATION: m φ H and inflaton starts to oscillate near origin and produce particles. Let there be light - dark vacuumlike state exploded and created hot universe: BIG BANG!!! (Re)heating temperature is model dependent, most probably is not large, T rh < E GUT GeV. No unwanted magnetic monopoles. Initial hot universe might be far from thermal equilibrium. 87

88 Cosmological charge asymmetry. Universe is particle-antiparticle asymmetric, at least in our neighborhood: β = N B N B N γ = (6 ± 1) a quarter of century ago β = 10 9±1, some improvement of accuracy! 88

89 Sufficient inflation is incompatible with conserved baryons. It is necessary Ht inf > 60. If B is conserved then only Ht inf (4 5) is allowed. Inflation proves that baryonic charge is nonconserved. 89

90 BARYOGENESIS. Three Sakharov conditions: 1. Non-conservation of baryons, theoretically predicted (EW, GUT); the only experimental piece of data is cosmology: we exist, ergo baryons are not conserved. 2. Breaking of C and CP, experimentally established. 3. Deviation from thermal equilibrium, always present in the early universe due to massive particles or first order phase transitions. 90

91 All three Sakharov conditions are fulfilled in MSM but the asymmetry is about 10 orders of magnitude below the observed value or even less, because heavy Higgs makes 1st order p.t. improbable. 91

92 Other scenarios: 1. Baryo-thru-lepto. 2. SUSY flat directions and baryonic condensate. 3. Evaporation of primordial black holes. 4. Many others... difficult to distinguish between them because only one number β is to be explained. 92

93 Scenarios with non-constant β. Isocurvature fluctuations at small scales, say, Mpc are not forbidden by CMBR. Even β < 0, i.e. astronomically large domains of antimatter are allowed. Search for cosmic antimatter may shed light on the baryogenesis scenario. Anyhow, new physics is necessary. 93

94 BBN, a cornerstone of SCM Well established physics, T = MeV, t = sec. Abundances of 2 H, 3 He, 4 He, and 7 Li, differing by 9 orders of magnitude, are successfully explained. 94

95 Figure 1: He 4, D, He 3 and Li 7 predicted by the standard BBN. Boxes indicate the observed light element abundances (smaller boxes: 2σ statistical errors; larger boxes: ±2σ statistical and systematic errors). The vertical band is the CMB measure of the cosmic baryon density. 95

96 Different groups present lower 4 He, N (eff) ν = 2.5. New physics or low accuracy and systematics? 96

97 Hydrogen recombination and CMBR. Perfect equilibrium Planck spectrum, T = ± K, n γ = ± 0.5 cm 3, Ω γ = (4.9 ± 0.5) Small angular fluctuations of temperature, snapshot of the universe at z 10 3, allow to measure cosmological parameters. 97

98 large angles one degree arcminutes 4x10-10 acoustic oscillations l(l+1)c l /2π 2x10-10 Sachs-Wolfe plateau Total Scalar 0 Tensor l 1000 Figure 2: Angular power spectrum for adiabatic initial perturbations and typical cosmological parameters. The scalar and tensor contributions to the anisotropies are also shown. 98

99 (l+1) C l /2π (µk 2 ) l (l+1) C l /2π (µk 2 ) Angular Scale Λ-CDM All Data WMAP CBI ACBAR Reionization TT Cross Power Spectrum TE Cross Power Spectrum Multipole moment (l) Figure 3: Temperature-temperature (TT) and temperature-polarization TE power spectra. The best fit ΛCDM model is also shown. Alignment and small amplitudes of low multipoles. Evil axis? Cosmic variance. 99

100 Measurements of angular spectrum of CMBR and power spectrum of LSS (SDSS, 2dFGRS) allow to determine all basic cosmological parameters and the type of perturbation spectrum with per cent level accuracy. 100

101 CONCLUSION Cosmology proves that there is NEW PHYSICS: New fields and particles exist (inflaton, DM, DE?). Baryonic number is not conserved and new fields inducing baryogenesis are necessary. New mechanisms of CP violation could operate in the early universe, maybe much different from the standard one. 101

102 Dark antigravitating energy. QCD measures vacuum energies of quark and gluon condensate which have vacuum energy 50 orders of magnitude larger than that observed. Who killed it? Some compensating agent must exist! 102

103 Quite natural to expect that ρ vac is not completely compensated and ρ ρ c Realistic model is needed, it can indicate what is w: is it (-1) or different. Accurate measurements of w are important. 103

104 FUTURE OBSERVATIONS: Planck mission, in two years from now? SNAP Polarization of CMBR and B(PS) modes, gravitational waves. More precise determination of power spectrum at smaller scales, isocurvature fluctuations? New measurements, new discoveries, new problems, new physics. 104

105 One should be aware of Pandora box of consequences if sacred principles are destroyed. If God does not exist anything is allowed. from Karamazov brothers, F.M. Dostoevsky. 105