The dark universe SFB – Transregio Bonn – Munich - Heidelberg.

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The dark The dark universe universe SFB – Transregio SFB – Transregio Bonn – Munich - Bonn – Munich - Heidelberg Heidelberg

Transcript of The dark universe SFB – Transregio Bonn – Munich - Heidelberg.

Page 1: The dark universe SFB – Transregio Bonn – Munich - Heidelberg.

The dark The dark universeuniverseSFB – TransregioSFB – Transregio

Bonn – Munich - HeidelbergBonn – Munich - Heidelberg

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What is our universe What is our universe made of ?made of ?

quintessence ! fire , air,

water, soil !

Basic questions , high public interest !

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ΩΩmm + X = 1 + X = 1

ΩΩmm : 30% : 30%

ΩΩhh : 70% : 70% Dark EnergyDark Energy

?

Unification ofall interactions

Superstrings

Higher dimensions

Fundamentalorigin of mass scales

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Important predictions of Dark Important predictions of Dark EnergyEnergy

The expansion of the Universe

accelerates today !

Structure Structure formation : formation : OneOne primordial primordial

fluctuation- fluctuation- spectrumspectrum

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Baryon - PeakBaryon - Peak

SDSSSDSS

galaxy – galaxy – correlation –correlation –functionfunction

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Observing Dark EnergyObserving Dark Energy

needs understandingneeds understandingof cosmological role ofof cosmological role of

Dark Matter !Dark Matter !

central for our TRcentral for our TR

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Research fields of TR33Research fields of TR33

Origin of Dark Energy and Dark Matter

Dark Matter –Dark Energyconnection

Time history of

Dark Energy

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What is Dark Energy ?

Cosmological Constant or Quintessence ?

Help from observation !

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Cosmological ConstantCosmological Constant- Einstein -- Einstein -

Constant Constant λλ compatible with all compatible with all symmetriessymmetries

No time variation in contribution to No time variation in contribution to energy densityenergy density

Why so small ? Why so small ? λλ/M/M44 = 10 = 10-120-120

Why important just today ?Why important just today ?

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Cosm. Const. | Quintessence static | dynamical

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Cosmological mass scalesCosmological mass scalesOnly ratios of mass scales are observable !Only ratios of mass scales are observable !

homogeneous dark energy: homogeneous dark energy: ρρhh/M/M44 = 6.5 = 6.5 10ˉ¹²¹10ˉ¹²¹

matter: matter: ρρmm/M/M4= 3.5 10ˉ¹²¹= 3.5 10ˉ¹²¹

ρρm,rm,r/M/M44 ~ ~ t t -2-2

For matter : huge age of For matter : huge age of universe universe

small ratiosmall ratio

Same explanation for small dark Same explanation for small dark energy energy ??

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Realization :

Scalar field,Quintessence,K-essence, ..

New interaction !

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The nature ofDark Energy determinesthe future of theUniverse …

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Themes of this TRThemes of this TR

Dark EnergyDark Energy Static or dynamic ?Static or dynamic ? Origin of Dark EnergyOrigin of Dark Energy Dark Matter – cosmological contextDark Matter – cosmological context Interactions Dark Energy – Dark Interactions Dark Energy – Dark

MatterMatter Structure formation – cosmological Structure formation – cosmological

aspectsaspects

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Theory – simulation - Theory – simulation - observationobservation

Complete chain from basic theory to observationComplete chain from basic theory to observation Cosmological expertise from theoretical particle Cosmological expertise from theoretical particle

physics and astrophysics : physics and astrophysics : synergysynergy needs effort !needs effort !

Observational approaches Observational approaches : complementary: complementary Leading role in large surveys:Leading role in large surveys: CMB : CMB : PlanckPlanck satellite satellite

Lensing, Galaxy Power Spectra and Galaxy Clusters : Lensing, Galaxy Power Spectra and Galaxy Clusters :

OmegaCam, VirusOmegaCam, Virus

Galaxy Clusters : Galaxy Clusters : X-rays, APEX , SupernovaeX-rays, APEX , Supernovae surveys surveys

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Theory – simulation - Theory – simulation - observationobservation

Theory Theory : basic and phenomenological approaches: basic and phenomenological approaches

Includes central areas where new insights and ideas Includes central areas where new insights and ideas on Dark Energy may come from : on Dark Energy may come from :

Superstrings, higher dimensions, dilatation Superstrings, higher dimensions, dilatation symmetrysymmetry

Simulations Simulations : leading groups: leading groups

Dynamical Dark Energy not much studied yetDynamical Dark Energy not much studied yet

New numerical challenges for inclusion of Dark New numerical challenges for inclusion of Dark Energy –Dark Matter coupling ( fluctuations of scalar Energy –Dark Matter coupling ( fluctuations of scalar field ) field )

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Interface theory-Interface theory-observationobservationmilestonesmilestones

Time history of Dark EnergyTime history of Dark Energy

Determination of Determination of cosmological Dark Matter characteristics and cosmological Dark Matter characteristics and possible coupling to Dark Energy from possible coupling to Dark Energy from

comparison ofcomparison of observation and simulations of dark matter observation and simulations of dark matter

structuresstructures

Standard model for cosmology ? !Standard model for cosmology ? !

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Time history of dark Time history of dark energyenergy

Measure this curve !Measure this curve !

h

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TR working groupsTR working groups

Time history of dark energyTime history of dark energy Cosmological dark matter propertiesCosmological dark matter properties Simulations of the universeSimulations of the universe Cosmological information from structure Cosmological information from structure

formationformation Gravitational lensing as probe for cosmologyGravitational lensing as probe for cosmology Cosmology from galaxy distributionsCosmology from galaxy distributions Theory of Dark EnergyTheory of Dark Energy Theory of Dark MatterTheory of Dark Matter

some well focused – some more vague

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Additional strength of TRAdditional strength of TR

Close connection with Close connection with several high level organized several high level organized graduate schoolsgraduate schools

Bonn International Graduate School Bonn International Graduate School Bonn IMPRS AstronomyBonn IMPRS Astronomy Heidelberg IMPRS “Astronomy and Heidelberg IMPRS “Astronomy and

cosmic physics”cosmic physics” Munich IMPRS “Astrophysics”Munich IMPRS “Astrophysics”

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Postdocs and PhD students :

central for activity of TR !

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Early Dark EnergyEarly Dark Energy

A few percent in A few percent in the early the early UniverseUniverse

Not possible for Not possible for a cosmological a cosmological constantconstant

M.Doran , CW : B1

1σ and 2σ limits

Doran,Karwan,..

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Simple parameterization of Simple parameterization of time-dependent dark energy time-dependent dark energy

fractionfraction

Dark Energy during structure formation

CMB,SN,SDSS

Supernovae , Riess et al.

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A few percent Early Dark A few percent Early Dark EnergyEnergy

If linear power spectrum fixed today If linear power spectrum fixed today ( ( σσ8 8 ) :) :

More Structure at More Structure at high z !high z !

Bartelmann,Doran,…Bartelmann,Doran,…

Early quintessence slows down the Early quintessence slows down the growth of structuregrowth of structure

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Cluster number relative to ΛCDM

Two models with 4% Dark Energy during structure formation

Fixed σ8 ( normalization dependence ! )

Little Early Dark Energy can make Little Early Dark Energy can make large effect !large effect !

More clusters athigh redshift

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Challenge :

Simple, robust,model- and parameterization-independentstatements !

Reliable errors !