Transcript pptx
Cosmology Cosmology Where are we ? 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 BASE LCDM MODEL (Planck + lensing+WP + HL) PLANCK promised us precision cosmology… (1993) BASE LCDM MODEL (Planck + lensing+WP + HL) P.Natoli Parameter Value (68%) Wbh2 0.02218±0.00026 Wch2 0.1186±0.0022 100q* (acoustic scale at recombination) 1.04144±0.00061 (~ 500 parts per million accuracy) t 0.090±0.014 (WMAP “seeded”) ln(1010As) 3.087±0.024 ns 0.9614±0.0063 (<1 at > 5 s) H0 67.9±1.0 WL 0.693±0.013 s8 0.8233±0.097 zre 11.1±1.1 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…) More than primary Cl… • Cl -> structures @ z ~ 1000 • Lensing detected ~ 25 σ (after ACT) • Lensing -> structures @ z ~ 2 (consistent with predictions of ∧CDM…) A.Benoît-Levy More CMB than with Planck… More CMB than with Planck… • Cl @ l < 9000 • Fist lensing detection • SZ Clusters M.Niemack More than CMB, with Planck… More than CMB… M.Lopez-Caniego Esquisite full sky mm & sub-mm survey with more than 25 000 sources More than CMB… New class of objects at high redshift L.Montier More than CMB… Tension between CMB and clusters in Planck More than CMB… B.Kirk Optical data to calibrate the Y-M for clusters @ SALT CMB A Window on the early universe Constraining Inflation - n - running… - r -> B-modes J.Martin Physical Models Observables Single Field slow-roll Single Field with Features (ie non slow-roll) Single Field with noncanonical kinetic terms Multi field Scalar power spectrum … Entropic & adiabatic perturbations … Gravity waves … Non-Gaussianities … J.Martin ASPIC evidence: good models theory.physics.unige.ch/~ringeval/aspic.html The landscape beyond single field inflation… Physically motivated models can pass present day constraints: - Non linear sigma model (S.Koh) - Heavy field (M.Yamaguchi) Power spectrum. Isocurvature contribution. Non Gaussiannity Testing Inflation after the Planck era Testing Inflation after the Planck era Sequence is right… Testing Inflation after the Planck era Sequence is right… Will be painful… 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 Using voids… R.Triay … as rulers. What is anisotropies play a dynamical role? D.Witlshire, J.Ostrowski Testing Inflation after the Planck era Hunting B-modes… And the winners are … HI KMIII 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 LHC N. Kanaya Evidencing Dark matter LHC No signal yet… N. Kanaya Dark matter: entering into the controversies… You do not find dark matter because there is dark matter… M.Milgrom, B.Famey, L.Blanchet Debate … 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 BOSS @ 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 ? A.Blanchard Quintesssence ? Modified gravity ? C.Cress Small scale inhomogeneities ? D.Whitshire J.Ostrowski LTB ? Conclusion We are waiting for the next conference in Qui Nhon to monitor progresses Conclusion We are waiting for the next conference in Qui Nhon to monitor progresses Thanks to the organisers and specially to Jean Trân Thanh Vân