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Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN

Cosmology and the origin of structure. Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN. Rocky I : The universe observed Rocky II : The growth of cosmological structure Rocky III : Inflation and the origin of perturbations

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Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN

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  1. Cosmology and the origin of structure Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN Rocky I: The universe observed Rocky II: The growth of cosmological structure Rocky III: Inflation and the origin of perturbations Rocky IV: Dark matter and dark energy

  2. Rocky I: The universe observed • Cosmological parameters: • Power spectrum of large-scale structure: • Anisotropy of CMB:

  3. Theoretical developments (1917-1927) • Cosmological principle • Robertson-Walker metric • Expansion natural

  4. Observational developments (1912-1929)

  5. “… physically, he is a splendid specimen…” “… magnificent physique ….” “… manly …” “… loveable character …”

  6. University of Chicago 1909 National Champions

  7. Observational developments (1912-1929) • Cosmological principle (extragalactic astronomy) • Universe expands

  8. Hubble’s Discovery Paper - 1929 s

  9. Riess et al astro-ph/9410054 Hubble’s data

  10. Distance-luminosity relation

  11. Field equations

  12. Distance-luminosity relation light travels on geodesics

  13. Distance-luminosity relation Example: matter + lambda • Program: • measure via • input and calculate

  14. Type Ia supernova are standard candles Type Ia Supernovae Luminosity / Solar Luminosity -20 0 20 40 60 days

  15. Type Ia supernova Hubble diagram apparent magnitude [log(distance)] Perlmutter et al. (1998) redshift z

  16. cosmological constant, …some changing non-zero vacuum energy, … or some unknown systematic effect(s) WVACUUM maximum theoretical bliss WMATTER

  17. Newton Einstein normal scale factor a time accelerated scale factor a vacuum energy? time

  18. The accelerating universe? • Normal matter slows the expansion of the universe (deceleration). Gravity is attractive. • Negative pressure would push apart space. • “Vacuum energy” (the mass-energy density of • space) is positive, but its pressure is negative.

  19. cosmological constant, …some changing non-zero vacuum energy, … or some unknown systematic effect(s) WVACUUM • The case for L: • acceleration 2) large-scale structure maximum theoretical bliss WMATTER

  20. 2dF data

  21. cosmological constant, …some changing non-zero vacuum energy, … or some unknown systematic effect(s) WVACUUM • The case for L: • acceleration • 2) large-scale structure 3) age of the universe maximum theoretical bliss WMATTER

  22. t0 : age of the universe Chaboyer (2001) Cayrel (2001) First measurement of stellar uranium • white dwarf cooling • nucleocosmochronology • globular cluster evolution

  23. cosmological constant, …some changing non-zero vacuum energy, … or some unknown systematic effect(s) WVACUUM • The case for L: • acceleration • 2) large-scale structure • 3) age of the universe maximum theoretical bliss • 4) flatness • W 0 = 1 • WM = 0.3 • 1 - 0.3 = 0.7 WMATTER

  24. Flat universe Hu

  25. WB h2~ 0.02 QSO 1937-1009 Ly-a Tytler Tytler

  26. WM ~ 0.3 galaxy kinematics • 0 = 1 WM = 0.3 • 1 - 0.3 = 0.7 x-ray gas lensing

  27. Cosmo-illogical constant Mass density of space: Who ordered that? The unbearable lightness of nothing!

  28. Temperature of the universe

  29. The cosmic food chain (Wi) Radiation: 0.02% Visible matter: 0.1% Neutrinos: 0.1% Dark neutrons & protons: 9.78% Dark matter: 30% Dark energy: 60%

  30. Observer’s view of the universe NGC 6070 lumpy (inhomogeneous and anisotropic) full of stars, galaxies, clusters, ….

  31. Theorist’s view of the universe Actual image of dark matter smooth (homogeneous and isotropic) full of dark matter (and dark energy)

  32. Power spectrum • Assume there is an average density • Expand density contrast in Fourier modes • Autocorrelation function defines power spectrum

  33. Power spectrum sphere of radius R • Power spectrum related to rms fluctuations

  34. Power spectrum

  35. Observer’s view of the universe (fluctuations)

  36. Theorist’s view of the universe (isotropic)

  37. Angular correlation function,

  38. Angular power spectrum LAST CENTURY

  39. Angular power spectrum

  40. Angular power spectrum MAP expected precision

  41. Rocky I: The universe observed • Cosmological parameters: • Power spectrum of large-scale structure: • Anisotropy of CMB:

  42. Cosmology and the origin of structure Academic Training Lectures Rocky Kolb Fermilab, University of Chicago, & CERN Rocky I: The observed universe Rocky II: The growth of cosmological structure Rocky III: Inflation and the origin of perturbations Rocky IV: Dark matter and dark energy

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