1. Scanning Inflation and Reheating Bottom-up approach to inflation: reconstruction of acceleration trajectories Top-down approach to inflation: seeks to embed it in fundamental theory Lev Kofman, CITA Cosmo05, Bonn September 1, 2005

2. Early Universe Inflation Scale factor time Realization of Inflation

3. Particlegenesis time Inflation no entropy no temperature BANG

5. Resonant Preheating in Chaotic Inflation

6. Classical Quantum Decay of inflaton and preheating after inflation movie Felder, LK, Peloso,05

7. Classical Quantum Decay of inflaton and preheating after inflation

9. inflation Hot FRW Initial conditions from Inflation

10. Modulated Fluctuations Light field at inflation Inflation radiation LK03;Dvali et al,03

11. Modulated fluctuations in Chaotic Inflation Podolsky, Felder, LK,Peloso hep-ph/0507096

12. 4 dimensional Inflation predicts No classical inhomogeneities from the past Scale free gaussian fluctuations of all light scalars No vector perturbations Scalar (almost scale free gaussian) metric perturbations Tensor (scale free gaussian) metric perturbations Creation of all SM particles in preheating/thermalization

13. Inflation in the context of ever changing fundamental theory 1980 2000 1990 -inflationOld Inflation New Inflation Chaotic inflation Double Inflation Extended inflation DBI inflation Super-natural Inflation Hybrid inflation SUGRA inflation SUSY F-term inflation SUSY D-term inflation SUSY P-term inflation Brane inflation K-flation N-flation Warped Brane inflation inflation Power-law inflation Tachyon inflation Racetrack inflation Assisted inflation

14. Search for inflaton with branes in extra dimensions 4-dim picture Dvali,Tye 98 Prototype of hybrid inflation

15. Compactification of inner dimensions with branes Old string theory New phenomenology Strongly warped 5d geometry Randal, Sundrum 99

16. Stabilization of Inner dimensions and moduli in string theory

18. Realization of String Theory Inflation on the ground of KKLT throat warped geometry Mobile brane modulated fluctuations Conformal coupling problem scalar field associated with angular position at KKLMMT03 Warped brane inflation Realization of warped brane inflation with conformal inflaton

19. Realization of String Theory Chaotic Inflation Mobile brane Chaotic inflation Mukohyama, LK 05

20. Reheating after String Theory Inflation Barnaby, Burgess, Cline, hep-th/0412095 LK, Yi, hep-th/0507257 Frey, Mazumdar, Myers, hep-th/0508139 Chialva, Shiu, Underwood, hep-th/0508229

21. Open strings between branes are unstable End point of inflation BANG SM particles Closed strings Unstable KK modes Long-living KK modes related to inner isometries LK, Yi 05

23. string theorist CY AdS 3+1 FRW Fluctuations in Cosmology with Compactification

24. string theorist CY AdS 3+1 FRW Fluctuations in Cosmology with Compactification CY cosmologist

25. string theorist Practical cosmologist CY AdS CY +fluctuations 3+1 FRW 3+1 FRW +fluctuations Fluctuations in Cosmology with Compactification CY cosmologist

26. KK story KK particles are thermalized first SM particles are thermalized much later KK from M with isometries are stable No complete decya KK particles freeze out

27. 4 dim Inflation in 10dim String Theory predicts All what 4 dim inflation predicts Scale free gaussian fluctuations of many light scalars Creation of non-SM particles (KK modes) in reheating/thermalization Short-wavelength gravitational radiation Modulated cosmological fluctuations String theory Cosmic strings

28. Scanning Inflation R.Bond, C.Contaldi, A.Frolov, L.Kofman T.Souradeep P.Vandrevange Bottom-up

29. Ensemble of Inflationary trajectories Chebyshev decomposition Space of models opens wide

32. Observational constraints on trajectories Markov Chain Monte Carlo

33. Degeneracy of the Potential Reconstruction

35. Reconstruction of Inflationary Trajectory

36. Cosmic Numerology: CMBall + LSS, stable & consistent pre-WMAP1 & post- WMAP1 (BCP03), Jun03 data (BCLP04), CMBall+CBIpol04, CMBall+Boom03+LSS Jul’21 05, CMBall Jul05 LSS=2dF, SDSS (weak lensing, cluster abundances); also HST, SN1a A s = 22 +- 3 x 10 -10 n s =.95 +-.02 (.97 +-.02 with tensor) (+-.004 PL1) A t / A s < 0.36 95% CL (+-.02 PL2.5+Spider) dn s /dln k = -.07 +-.04 to -.05 +-.03 (+-.005 P1) -.002 +-.01 (+Lya McDonald etal 04) (A iso / A s < 0.3 large scale, < 3 small scale n iso = 1.1+-.6) The Parameters of Cosmic Structur Formation