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Cosmology

Cosmology. Where are we ?. Cosmology. CMB. P.Natoli. 2009. Planck. Intensive robustness tests ( M.Lejeune ) Available on line : http://pla.esac.esa.int/pla/aio/ planckProducts.html Impressive power for Cosmology.

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Cosmology

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  1. Cosmology

  2. Where are we ? Cosmology

  3. CMB P.Natoli 2009 Planck

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

  5. BASE LCDM MODEL (Planck + lensing+WP+ HL) PLANCK promised us precisioncosmology… (1993)

  6. BASE LCDM 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 • Impressivepower for Cosmology (remembercosmology in 1993…)

  8. Cl -> structures @ z ~ 1000 • Lensingdetected~ 25 σ (after ACT) • Lensing -> structures @ z ~ 2 (consistent withpredictions of ∧CDM…) More thanprimary Cl… A.Benoît-Levy

  9. More CMB thanwith Planck…

  10. Cl @ l < 9000 • Fistlensingdetection • SZ Clusters More CMB thanwith Planck… M.Niemack

  11. More than CMB,with Planck…

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

  13. New class of objectsathighredshift More than CMB… L.Montier

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

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

  16. Constraining Inflation • n • running… • r -> B-modes CMBA Window on the earlyuniverse J.Martin

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

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

  19. Physicallymotivatedmodelscanpasspresentdayconstraints: - Non linear sigma model (S.Koh) • Heavy field (M.Yamaguchi) Power spectrum. Isocurvature contribution. Non Gaussiannity The landscapebeyond single field inflation…

  20. Testing Inflation after the Planck era

  21. Sequenceis right… Testing Inflation after the Planck era

  22. Sequenceis right… Will bepainful… Testing Inflation after the Planck era

  23. Primordial non-gaussianityMost inflationarymodelspredict smallbut modeldependent deviationsfromGaussianity M.Liguori

  24. Primordial non-gaussianity

  25. Y.Fantaye Testinganisotropy

  26. D.Witlshire Testinganisotropy

  27. Using voids… R.Triay … as rulers.

  28. D.Witlshire, J.Ostrowski Whatis anisotropies play a dynamicalrole?

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

  30. And the winners are … HI KMIII 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 biggame…

  37. EvidencingDarkmatter Conforting the standard model (∧CDM)

  38. Accelerator searches Direct detection Indirect detection Evidencingdarkmatter

  39. P.Tinyakov EvidencingDarkmatter

  40. F. Cafagna EvidencingDarkmatter

  41. F. Cafagna EvidencingDarkmatter

  42. F. Cafagna EvidencingDarkmatter

  43. AMS: Cosmic rays W. Gillard EvidencingDarkmatter

  44. DM particle in the room… B. Serfass EvidencingDarkmatter

  45. B. Serfass EvidencingDarkmatter

  46. LHC N. Kanaya EvidencingDarkmatter

  47. LHC N. Kanaya EvidencingDarkmatter No signal yet…

  48. You do not finddarkmatterbecausethereisdarkmatter… Debate … M.Milgrom, B.Famey, L.Blanchet Darkmatter: enteringinto the controversies…

  49. We are all living in an accelerateduniverse… There is no observationalreason to go beyond∧ Darkenergy: beforeenteringinto the controversies…

  50. Darkenergy M.Betoule

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