the dark universe sfb – transregio bonn – munich - heidelberg
TRANSCRIPT
The dark The dark universeuniverseSFB – TransregioSFB – Transregio
Bonn – Munich - HeidelbergBonn – Munich - Heidelberg
What is our universe What is our universe made of ?made of ?
quintessence ! fire , air,
water, soil !
Basic questions , high public interest !
ΩΩmm + X = 1 + X = 1
ΩΩmm : 30% : 30%
ΩΩhh : 70% : 70% Dark EnergyDark Energy
?
Unification ofall interactions
Superstrings
Higher dimensions
Fundamentalorigin of mass scales
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
Baryon - PeakBaryon - Peak
SDSSSDSS
galaxy – galaxy – correlation –correlation –functionfunction
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
Research fields of TR33Research fields of TR33
Origin of Dark Energy and Dark Matter
Dark Matter –Dark Energyconnection
Time history of
Dark Energy
What is Dark Energy ?
Cosmological Constant or Quintessence ?
Help from observation !
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 ?
Cosm. Const. | Quintessence static | dynamical
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 ??
Realization :
Scalar field,Quintessence,K-essence, ..
New interaction !
The nature ofDark Energy determinesthe future of theUniverse …
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
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
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 )
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 ? !
Time history of dark Time history of dark energyenergy
Measure this curve !Measure this curve !
h
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
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”
Postdocs and PhD students :
central for activity of TR !
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,..
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.
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
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
Challenge :
Simple, robust,model- and parameterization-independentstatements !
Reliable errors !