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The dark universe

The dark universe. SFB – Transregio Bonn – Munich - Heidelberg. What is our universe made of ?. fire , air, water, soil !. quintessence !. Basic questions , high public interest !. Ω m + X = 1 Ω m : 30% Ω h : 70% Dark Energy. Unification of all interactions Superstrings

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The dark universe

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

  2. What is our universe made of ? fire , air, water, soil ! quintessence ! Basic questions , high public interest !

  3. Ωm + X = 1 Ωm : 30% Ωh : 70% Dark Energy Unification of all interactions Superstrings Higher dimensions Fundamental origin of mass scales ?

  4. Important predictions of Dark Energy The expansion of the Universe accelerates today ! Structure formation : One primordial fluctuation- spectrum

  5. Baryon - Peak SDSS galaxy – correlation – function

  6. Observing Dark Energyneeds understandingof cosmological role ofDark Matter !central for our TR

  7. Research fields of TR33

  8. What is Dark Energy ? Cosmological Constant or Quintessence ? Help from observation !

  9. Cosmological Constant- Einstein - • Constant λ compatible with all symmetries • No time variation in contribution to energy density • Why so small ? λ/M4 = 10-120 • Why important just today ?

  10. Cosm. Const. | Quintessence static | dynamical

  11. Cosmological mass scales Only ratios of mass scales are observable ! homogeneous dark energy: ρh/M4 = 6.5 10ˉ¹²¹ matter: ρm/M4= 3.5 10ˉ¹²¹ ρm,r/M4~ t -2 For matter : huge age of universe small ratio Same explanation for small dark energy ?

  12. Realization : Scalar field, Quintessence, K-essence, .. New interaction !

  13. The nature of Dark Energy determines the future of the Universe …

  14. Themes of this TR • Dark Energy • Static or dynamic ? • Origin of Dark Energy • Dark Matter – cosmological context • Interactions Dark Energy – Dark Matter • Structure formation – cosmological aspects

  15. Theory – simulation - observation • Complete chain from basic theory to observation • Cosmological expertise from theoretical particle physics and astrophysics : synergyneeds effort ! • Observational approaches : complementary • Leading role in large surveys: CMB : Planck satellite Lensing, Galaxy Power Spectra and Galaxy Clusters : OmegaCam, Virus Galaxy Clusters : X-rays, APEX , Supernovae surveys

  16. Theory – simulation - observation • Theory : basic and phenomenological approaches Includes central areas where new insights and ideas on Dark Energy may come from : Superstrings, higher dimensions, dilatation symmetry • Simulations : leading groups Dynamical Dark Energy not much studied yet New numerical challenges for inclusion of Dark Energy –Dark Matter coupling ( fluctuations of scalar field )

  17. Interface theory-observationmilestones • Time history of Dark Energy • Determination of cosmological Dark Matter characteristics and possible coupling to Dark Energy from comparison of observation and simulations of dark matter structures • Standard model for cosmology ? !

  18. Time history of dark energy h Measure this curve !

  19. TR working groups • Time history of dark energy • Cosmological dark matter properties • Simulations of the universe • Cosmological information from structure formation • Gravitational lensing as probe for cosmology • Cosmology from galaxy distributions • Theory of Dark Energy • Theory of Dark Matter some well focused – some more vague

  20. Additional strength of TR Close connection with several high level organized graduate schools • Bonn International Graduate School • Bonn IMPRS Astronomy • Heidelberg IMPRS “Astronomy and cosmic physics” • Munich IMPRS “Astrophysics”

  21. Postdocs and PhD students : central for activity of TR !

  22. Early Dark Energy A few percent in the early Universe Not possible for a cosmological constant M.Doran , CW : B1 1σ and 2σ limits Doran,Karwan,..

  23. Simple parameterization of time-dependent dark energy fraction CMB,SN,SDSS Supernovae , Riess et al. Dark Energy during structure formation

  24. A few percent Early Dark Energy If linear power spectrum fixed today ( σ8 ) : More Structure at high z ! Bartelmann,Doran,… Early quintessence slows down the growth of structure

  25. Little Early Dark Energy can make large effect ! Cluster number relative to ΛCDM More clusters at high redshift Two models with 4% Dark Energy during structure formation Fixed σ8 ( normalization dependence ! )

  26. Challenge : Simple, robust, model- and parameterization- independent statements ! Reliable errors !

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