cosmology. where are we ? cosmology cmb cmb p.natoli 2009 planck

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