1. Cosmology

2. Where are we ? Cosmology

3. CMB CMB P.Natoli 2009 Planck

4.  Intensive robustness tests (M.Lejeune) Available on line : http://pla.esac.esa.int/pla/aio/planckProducts.html  Impressive power for Cosmology

5. BASE  CDM MODEL (Planck + lensing+WP + HL) PLANCK promised us precision cosmology… (1993)

6. ParameterValue (68%) bh2bh2 0.02218±0.00026 ch2ch2 0.1186±0.0022 100  * (acoustic scale at recombination) 1.04144±0.00061 (~ 500 parts per million accuracy)  0.090±0.014 (WMAP “seeded”) ln(10 10 A s )3.087±0.024 nsns 0.9614±0.0063 ( 5  ) H0H0 67.9±1.0  0.693±0.013 88 0.8233±0.097 z re 11.1±1.1 BASE  CDM MODEL (Planck + lensing+WP + HL) P.Natoli

7.  Intensive robustness tests (M.Lejeune) Available on line : http://pla.esac.esa.int/pla/aio/planckProducts.html  Impressive power for Cosmology (remember cosmology in 1993…)

8. More than primary Cl… More than primary Cl… Cl -> structures @ z ~ 1000 Cl -> structures @ z ~ 1000 Lensing detected ~ 25 σ (after ACT) Lensing detected ~ 25 σ (after ACT) Lensing -> structures @ z ~ 2 (consistent with predictions of ∧ CDM…) Lensing -> structures @ z ~ 2 (consistent with predictions of ∧ CDM…) A.Benoît-Levy

9. More CMB than with Planck… More CMB than with Planck…

10. Cl @ l < 9000 Cl @ l < 9000 Fist lensing detection Fist lensing detection SZ Clusters SZ Clusters M.Niemack

11. More than CMB, with Planck… More than CMB, with Planck…

12. More than CMB… More than CMB… M.Lopez-Caniego Esquisite full sky mm & sub-mm survey with more than 25 000 sources

13. More than CMB… More than CMB… L.Montier New class of objects at high redshift

14. More than CMB… More than CMB… Tension between CMB and clusters in Planck

15. More than CMB… More than CMB… Optical data to calibrate the Y-M for clusters @ SALT B.Kirk

16. Constraining Inflation - n - running… - r -> B-modes CMB A Window on the early universe J.Martin

17. Entropic & adiabatic perturbations Scalar power spectrum Gravity waves Non-Gaussianities Single Field slow-roll Single Field with non- canonical kinetic terms Multi field Single Field with Features (ie non slow-roll) Physical Models Observables … … … … J.Martin

18. ASPIC evidence: good models theory.physics.unige.ch/~ringeval/aspic.html

19. Physically motivated models can pass present day constraints: - Non linear sigma model (S.Koh) - Heavy field (M.Yamaguchi) Power spectrum. Power spectrum. Isocurvature contribution. Isocurvature contribution. Non Gaussiannity Non Gaussiannity The landscape beyond single field inflation…

20. Testing Inflation after the Planck era

21. Sequence is right… Testing Inflation after the Planck era

22. Sequence is right… Will be painful… Testing Inflation after the Planck era

23. Primordial non-gaussianity Most inflationary models predict small but model dependent deviations from Gaussianity Primordial non-gaussianity Most inflationary models predict small but model dependent deviations from Gaussianity M.Liguori

24. Primordial non-gaussianity

25. Testing anisotropy Y.Fantaye

26. Testing anisotropy D.Witlshire

27. … as rulers. R.Triay Using voids…

28. What is anisotropies play a dynamical role? D.Witlshire, J.Ostrowski

29. Hunting B-modes… Testing Inflation after the Planck era

30. And the winners are … KMIII HI J.Martin

31. And the winners are … J.Martin

32. Hunting B-modes… M.Lopes-Caniego

33. Hunting B-modes… M.-A. Bigot-Sazy

34. Hunting B-modes… H.Nguyen

35. Hunting B-modes… H.Nguyen

36. BICEP1,2,3,Keck-Array r = 0.01 is the big game…

37. Conforting the standard model ( ∧ CDM) Evidencing Dark matter

38. Evidencing dark matter Accelerator searches Direct detection Indirect detection

39. Evidencing Dark matter P.Tinyakov

40. Evidencing Dark matter F. Cafagna

41. Evidencing Dark matter F. Cafagna

42. Evidencing Dark matter F. Cafagna

43. Evidencing Dark matter AMS: Cosmic rays W. Gillard

44. Evidencing Dark matter DM particle in the room… B. Serfass

45. Evidencing Dark matter B. Serfass

46. Evidencing Dark matter N. Kanaya LHC

47. Evidencing Dark matter N. Kanaya No signal yet… LHC

48. Dark matter: entering into the controversies… You do not find dark matter because there is dark matter… Debate … M.Milgrom, B.Famey, L.Blanchet

49. Dark energy: before entering into the controversies… We are all living in an accelerated universe… There is no observational reason to go beyond ∧

50. Dark energy M.Betoule

51. Dark energy: galaxy surveys M.Betoule

52. Dark energy: redshift surveys Boss I, II, III, DESI… S.Bailey

53. Dark energy: redshift surveys Boss I, II, III, DESI… S.Bailey

54. Dark energy: redshift surveys Boss I, II, III, DESI… S.Belay

55. Dark energy: Lα clouds with BOSS @ z ~ 2.3 G.Rossi

56. Dark energy: the LSST perspective F.Villa

57. Dark energy: the LSST perspective F.Villa

58. Dark energy: the LSST perspective F.Villa

59. Dark energy: the SKA perspective C.Cress

60. Dark energy: the SKA perspective C.Cress

61. Dark energy: entering into the controversies… (weak) R.Triay

62. Dark energy: Nature & Controversies Quantum vacuum ? Quintesssence ? Modified gravity ? Small scale inhomogeneities ? LTB ? A.Blanchard C.Cress D.Whitshire J.Ostrowski

63. We are waiting for the next conference in Qui Nhon to monitor progresses Conclusion

64. Thanks to the organisers and specially to Jean Trân Thanh Vân Conclusion