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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
BASE LCDM MODEL (Planck + lensing+WP + HL)
PLANCK promised us precision cosmology… (1993)
Parameter Value (68%)Wbh2 0.02218±0.00026Wch2 0.1186±0.0022100q* (acoustic scale at recombination)
1.04144±0.00061 (~ 500 parts per million accuracy)
t 0.090±0.014 (WMAP “seeded”)
ln(1010As) 3.087±0.024ns 0.9614±0.0063 (<1 at > 5
s) H0 67.9±1.0WL 0.693±0.013s8 0.8233±0.097zre 11.1±1.1
BASE LCDM MODEL (Planck + lensing+WP + HL)
P.Natoli
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 thanwith 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…
L.MontierNew class of objects at high redshift
More than CMB…
Tension between CMB and clusters in Planck
More than CMB…
Optical data to calibrate the Y-M for clusters @ SALT
B.Kirk
Constraining Inflation- n- running…- r -> B-modes
CMBA Window on the early
universe
J.Martin
Entropic & adiabatic perturbations
Scalar power spectrum
Gravity waves
Non-Gaussianities
Single Fieldslow-roll
Single Fieldwith non-canonical
kinetic termsMulti field
Single Fieldwith Features
(ie non slow-roll)
PhysicalModels
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. Isocurvature contribution. 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 modeldependent 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 searchesDirect 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 raysW. Gillard
Evidencing Dark matter
DM particle in the room… B. Serfass
Evidencing Dark matter
B. Serfass
Evidencing Dark matter
N. KanayaLHC
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 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 ?
Quintesssence ?
Modified gravity ?
Small scale inhomogeneities ?
LTB ?
A.Blanchard
C.Cress
D.WhitshireJ.Ostrowski
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
Conclusion
