1. SOME LIKE IT HOT: dynamical suppression of vacuum configurations in cosmology, and hot CMB A.O.Barvinsky Theory Department, Lebedev Physics Institute, Moscow

2. vs eternal inflation, self-reproduction and multiverse picture Initial quantum state

3. Two known prescriptions for a pure initial state: no-boundary wavefunction (Hartle-Hawking); “tunneling” wavefunction ( Linde, Vilenkin, Rubakov, Zeldovich-Starobinsky, …)

4. Euclidean spacetime Hyperbolic nature of the Wheeler-DeWitt equation Euclidean action of quasi-de Sitter instanton with the effective  (slow roll)  inflatonother fields no tunneling, really: “birth from nothing” Semiclassical properties of the no-boundary/tunneling states Analytic continuation – Lorentzian signature dS geometry: Euclidean FRW -- de Sitter invariant (Euclidean) vacuum

5. Tunneling ( - ) : probability maximum at the maximum of the inflaton potential No-boundary ( + ) : probability maximum at the mininmum of the inflaton potential vs infrared catastrophe no inflation contradicts renormalization theory for + sign Beyond tree level: inflaton probability distribution: Both no-boundary (EQG path integral) and tunneling (WKB approximation) do not have a clear operator interpretation Eucidean effective action on S 4

6. We suggest a unified framework for the no-boundary and tunneling states in the form of the path integral of the microcanonical ensemble in quantum cosmology We apply it to the Universe dominated by: i) massless matter conformally coupled to gravity new (thermal) status of the no-boundary state; bounded range of the primordial  with band structure; dynamical elimination of vacuum no-boundary and tunneling states; inflation and thermal corrections to CMB power spectrum A.B. & A.Kamenshchik, JCAP, 09, 014 (2006) Phys. Rev. D74, 121502 (2006); A.B., Phys. Rev. Lett. 99, 071301 (2007)

7. Plan Cosmological initial conditions – density matrix of the Universe: microcanonical ensemble in cosmology initial conditions for the Universe via EQG statistical sum CFT driven cosmology: constraining landscape of  suppression of vacuum no-boundary and tunneling states inflation and generation of thermally corrected CMB spectrum

8. operators of the Wheeler-DeWitt equations Microcanonical density matrix – projector onto subspace of quantum gravitational constraints A.O.B., Phys.Rev.Lett. 99, 071301 (2007) Microcanonical ensemble in cosmology and EQG path integral constraints on initial value data – corner stone of any diffeomorphism invariant theory. Physical states: Statistical sum

9. Motivation: aesthetical (minimum of assumptions) Spatially closed cosmology does not have freely specifiable constants of motion. The only conserved quantities are the Hamiltonian and momentum constraints H , all having a particular value --- zero The microcanonical ensemble with is a natural candidate for the quantum state of the closed Universe – ultimate equipartition in the physical phase space of the theory --- Sum over Everything.

10. Lorentzian path integral representation for the microcanonical statistical sum: real axis Integration range: Functional coordinate representation of 3-metric and matter fields q and conjugated momenta p :

11. EQG density matrix D.Page (1986) Lorentzian path integral = Euclidean Quantum Gravity (EQG) path integral with the imaginary lapse integration contour: Euclidean metric Euclidean action of Euclidean metric and matter fields

12. on S 3 £ S 1 Spacetime topology in the statistical sum: including as a limiting (vacuum) case S 4 (thermal) S 3 topology of a spatially closed cosmology

13. Hartle-Hawking state as a vacuum member of the microcanonical ensemble: pinching a tubular spacetime density matrix representation of a pure Hartle-Hawking state – vacuum state of zero temperature T ~ 1/    (see below)

14. minisuperspace background quantum “matter” – cosmological perturbations: Euclidean FRW metric 3-sphere of a unit size scale factorlapse Disentangling the minisuperspace sector Path integral calculation:

15. quantum effective action of  on minisuperspace background Decomposition of the statistical sum path integral:

16. Origin of no-boundary/tunneling contributions No periodic solutions of effective equations with imaginary Euclidean lapse N (Lorentzian spacetime geometry). Saddle points exist for real N (Euclidean geometry): Deformation of the original contour of integration into the complex plane to pass through the saddle point with real N>0 or N<0 gauge equivalent N<0 gauge equivalent N>0 gauge (diffeomorphism) inequivalent!

17. sum over Everything (all solutions) will be suppressed dynamically!

18. Application to the CFT driven cosmology N s À 1 conformal fields of spin s=0,1,1/2  3H 2 -- primordial cosmological constant Assumption of N cdf conformally invariant, N cdf À 1, quantum fields and recovery of the action from the conformal anomaly and the action on a static Einstein Universe conformal time A.A.Starobinsky (1980); Fischetty,Hartle,Hu; Riegert; Tseytlin; Antoniadis, Mazur & Mottola; …… Conformal invariance  exact calculation of S eff

19. Gauss-Bonnet term Weyl term spin-dependent coefficients N s # of fields of spin s anomaly Einstein universe contribution

20. nonlocal (thermal) part classical part conformal anomaly part vacuum (Casimir) energy – from static EU -- coefficient of the Gauss-Bonnet term in the conformal anomaly Full quantum effective action on FRW background -- time reparameterization invariance (1D diffeomorphism) energies of field oscillators on S 3 inverse temperature

21. Effective Friedmann equation for saddle points of the path integral: amount of radiation constant “bootstrap” equation:  [a(  )] -- coefficient of the Gauss-Bonnet term in the conformal anomaly

22. k- folded garland, k=1,2,3,… 1- fold, k=1 Saddle point solutions --- set of periodic ( thermal) garland-type instantons with oscillating scale factor ( S 1 X S 3 ) and vacuum Hartle-Hawking instantons ( S 4 ) S4S4,....

23.     …  k – cosmological constant band for k-folded garland  C  Band structure of the bounded cosmological constant range   New QG scale at k  1: instantons with temperatures

24. Dynamical elimination of the vacuum no-boundary state: ( S 4 instanton solutions ) N  - N,   - , only vacuum S 4 instantons exist as saddle-point solutions Dynamical elimination of tunneling states: dominant anomaly contribution

25. pinching transition to statistical sum field identification arrow of time inherited from Lorentzian theory

26. Local bosonic action 1 UV renormalized and finite on a smooth manifold without identifications Fermions: Pauli principle

27. Inflationary evolution and “hot” CMB Lorentzian Universe with initial conditions set by the saddle-point instanton. Analytic continuation of the instanton solutions: Decay of a composite  exit from inflation and particle creation of conformally non-invariant matter: matter energy density Inflation via  as a composite operator – inflaton potential and a slow roll Expansion and quick dilution of primordial radiation

28. Primordial CMB spectrum with thermal corrections: additional reddening of the CMB spectrum thermal contribution physical scale standard red CMB spectrum

29. thermal part is negligible: contribution of higher conformal spins might be visible   per one degree of freedom ? 1 ?

30. SOME LIKE IT COOL

31. Conclusions Microcanonical density matrix of the Universe Euclidean quantum gravity path integral – unifying framework for the no- boundary and tunneling states Application to the CFT driven cosmology with a large # of quantum species – thermal version of the no-boundary state Dynamical elimination of vacuum no-boundary and tunneling states Initial conditions for inflation with a limited range of  -- cosmological landscape -- and generation of the thermal CMB spectrum

32. С ДНЕМ РОЖДЕНИЯ, МИСАО! HAPPY BIRTHDAY, MISAO! MANY PRODUCTIVE YEARS, GIFTED STUDENTS AND HAPPINESS TO YOUR FAMILY!