cosmology
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
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Cosmology
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Where are we ?
Cosmology
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CMB
P.Natoli
2009 Planck
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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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BASE LCDM MODEL (Planck + lensing+WP + HL)
PLANCK promised us precision cosmology… (1993)
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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
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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…)
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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
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More CMB thanwith Planck…
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More CMB than with Planck…
• Cl @ l < 9000• Fist lensing detection • SZ Clusters
M.Niemack
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More than CMB,with Planck…
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More than CMB…
M.Lopez-Caniego
Esquisite full sky mm & sub-mm survey with more than 25 000 sources
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More than CMB…
L.MontierNew class of objects at high redshift
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More than CMB…
Tension between CMB and clusters in Planck
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More than CMB…
Optical data to calibrate the Y-M for clusters @ SALT
B.Kirk
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Constraining Inflation- n- running…- r -> B-modes
CMBA Window on the early
universe
J.Martin
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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
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ASPIC evidence: good models
theory.physics.unige.ch/~ringeval/aspic.html
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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…
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Testing Inflation after the Planck era
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Sequence is right…
Testing Inflation after the Planck era
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Sequence is right…
Will be painful…
Testing Inflation after the Planck era
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Primordial non-gaussianity
Most inflationary models predict small but modeldependent deviations from Gaussianity
M.Liguori
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Primordial non-gaussianity
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Testing anisotropy Y.Fantaye
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Testing anisotropy D.Witlshire
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… as rulers.
R.Triay
Using voids…
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What is anisotropies play a dynamical role?
D.Witlshire, J.Ostrowski
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Hunting B-modes…
Testing Inflation after the Planck era
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And the winners are …
KMIII
HI
J.Martin
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And the winners are …
J.Martin
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Hunting B-modes…
M.Lopes-Caniego
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Hunting B-modes…
M.-A. Bigot-Sazy
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Hunting B-modes…
H.Nguyen
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Hunting B-modes…
H.Nguyen
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BICEP1,2,3,Keck-Array
r = 0.01 is the big game…
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Conforting the standard model
(∧CDM)
Evidencing Dark matter
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Evidencing dark matter
Accelerator searchesDirect detection
Indirect detection
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Evidencing Dark matter
P.Tinyakov
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Evidencing Dark matter
F. Cafagna
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Evidencing Dark matter
F. Cafagna
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Evidencing Dark matter
F. Cafagna
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Evidencing Dark matter
AMS: Cosmic raysW. Gillard
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Evidencing Dark matter
DM particle in the room… B. Serfass
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Evidencing Dark matter
B. Serfass
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Evidencing Dark matter
N. KanayaLHC
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Evidencing Dark matter
N. Kanaya
No signal yet…
LHC
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Dark matter: entering into the
controversies…
You do not find dark matter because there is dark matter…
Debate …
M.Milgrom, B.Famey, L.Blanchet
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Dark energy: before entering
into the controversies…
We are all living in an accelerated universe…
There is no observational reason to go beyond ∧
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Dark energy
M.Betoule
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Dark energy: galaxy surveys
M.Betoule
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Dark energy: redshift surveys
Boss I, II, III, DESI…S.Bailey
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Dark energy: redshift surveys
Boss I, II, III, DESI…S.Bailey
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Dark energy: redshift surveys
Boss I, II, III, DESI…S.Belay
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Dark energy: Lα clouds with BOSS @ z ~ 2.3
G.Rossi
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Dark energy: the LSST perspective
F.Villa
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Dark energy: the LSST perspective
F.Villa
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Dark energy: the LSST perspective
F.Villa
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Dark energy: the SKA perspective
C.Cress
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Dark energy: the SKA perspective
C.Cress
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Dark energy: entering into the controversies…
(weak)
R.Triay
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Dark energy: Nature & Controversies
Quantum vacuum ?
Quintesssence ?
Modified gravity ?
Small scale inhomogeneities ?
LTB ?
A.Blanchard
C.Cress
D.WhitshireJ.Ostrowski
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We are waiting for the next conference in Qui Nhon to monitor progresses
Conclusion
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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