Cosmology

Where are we ? Cosmology

CMB CMB P.Natoli 2009 Planck

 Intensive robustness tests (M.Lejeune) Available on line :  Impressive power for Cosmology

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

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

 Intensive robustness tests (M.Lejeune) Available on line :  Impressive power for Cosmology (remember cosmology in 1993…)

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

More CMB than with Planck… More CMB than with Planck…

l < 9000 l < 9000 Fist lensing detection Fist lensing detection SZ Clusters SZ Clusters M.Niemack

More than CMB, with Planck… More than CMB, with Planck…

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

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

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

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

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

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

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

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…

Testing Inflation after the Planck era

Sequence is right… Testing Inflation after the Planck era

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

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

Primordial non-gaussianity

Testing anisotropy Y.Fantaye

Testing anisotropy D.Witlshire

… as rulers. R.Triay Using voids…

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

Hunting B-modes… Testing Inflation after the Planck era

And the winners are … KMIII HI J.Martin

And the winners are … J.Martin

Hunting B-modes… M.Lopes-Caniego

Hunting B-modes… M.-A. Bigot-Sazy

Hunting B-modes… H.Nguyen

Hunting B-modes… H.Nguyen

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

Conforting the standard model ( ∧ CDM) Evidencing Dark matter

Evidencing dark matter Accelerator searches Direct detection Indirect detection

Evidencing Dark matter P.Tinyakov

Evidencing Dark matter F. Cafagna

Evidencing Dark matter F. Cafagna

Evidencing Dark matter F. Cafagna

Evidencing Dark matter AMS: Cosmic rays W. Gillard

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

Evidencing Dark matter B. Serfass

Evidencing Dark matter N. Kanaya LHC

Evidencing Dark matter N. Kanaya No signal yet… LHC

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

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

Dark energy M.Betoule

Dark energy: galaxy surveys M.Betoule

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

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

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

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

Dark energy: the LSST perspective F.Villa

Dark energy: the LSST perspective F.Villa

Dark energy: the LSST perspective F.Villa

Dark energy: the SKA perspective C.Cress

Dark energy: the SKA perspective C.Cress

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

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

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

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