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New Views on the Universe

New Views on the Universe. V èmes Rencontres du Vietnam August 2004. Angela V. Olinto Astronomy & Astrophysics Kavli Institute Cosmol. Phys. Enrico Fermi Institute University of Chicago. Much to celebrate!. Success of the Big Bang theory Flat Universe (Inflationary prediction)

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New Views on the Universe

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  1. New Views on the Universe Vèmes Rencontres du Vietnam August 2004 Angela V. Olinto Astronomy & Astrophysics Kavli Institute Cosmol. Phys. Enrico Fermi Institute University of Chicago

  2. Much to celebrate! • Success of the Big Bang theory • Flat Universe (Inflationary prediction) • Discovery of Universe’s Acceleration • Discovery of Neutrino mixing  mass • Gamma-ray Bursts Cosmolog.+ Counterparts • Black Holes in every galaxy! • TeV Gamma-ray Sources Many questions remain... Vèmes Rencontres du Vietnam 2004

  3. The Big Bang

  4. The Big Bang We live in a Homogeneous & Isotropic Universe described by (a Robertson-Walker metric & Friedmann’s equation derived from) Einstein’s General Relativity. It began 13.7 billion years ago, and is composed of... Celebrate Einstein Centennial!

  5. Evidence for Isotropy: The Microwave Sky! T = 2.725  0.002 K

  6. launched 1989

  7. b Big Bang Nucleosynthesis Theory vs. Observations: Remarkable agreement over 10 orders of magnitude in abundance variation Concordance region: b h2 = 0.02 For h=0.7, b = 0.04. Deuterium: strongest constraint 4He

  8. The Big Bang

  9. add Inflation and we can explain...

  10. Brief History of the Universe Inflation exponential expansion

  11. Homogeneity & Isotropy Horizon of observer B at time of decoupling A B Big Bang t=0 Us, today Photon Decoupling (Last Scattering Surface) t=300,000 yr CMB naturally appears isotropic

  12. V() Quantum Fluctuations of the `Inflaton’ Field ==> Density Perturbations  field V() space  field

  13. Today Scale grow 3000 Mpc 1 Mpc stretch inside outside inside Time Before inflation Radiation Domination Matter Domination During inflation Dark Energy Domination

  14. High-Resolution Simulations of Cold Dark Matter (CDM) Halos

  15. CMB Anisotropies tU =380,000 yr, T  10-5 T

  16. WMAP Precision Cosmology

  17. total = 1.02  0.02 FLAT!

  18. Inflation predicts: FLAT Universe

  19. Dark Energy? total =  +DM +b = 0.73, DM = 0.23, b = 0.04

  20. SnIa WMAP (h fix) LSS 2dF

  21. Radiation - Matter - Vacuum (Dark Energy?) (a) a-4 a-3 const a Early Universe today

  22. Expect dq/dz Riess et al. ApJLett 04, HST 16 SNIa

  23. Towards  = 1 closed expands forever recollapses open

  24. Much to celebrate! • Success of the Big Bang theory • Flat Universe (Inflationary prediction) • Discovery of Universe’s Acceleration • Discovery of Neutrino mixing  mass • Gamma-ray Bursts Cosmolog.+ Counterparts • Black Holes in every galaxy! • TeV Gamma-ray Sources

  25. Official detections by H.E.S.S. Crab Nebula (2003, 3 Tel.) - 54 sigma PKS 2155 (2003, 2 Tel.) - 45 sigma Mrk 421 (2004, 4 Tel.) - 71 sigma PSR B1259 (2004, 4 Tel.) - 8 sigma RX J1713 (2003, 2 Tel.) - 20 sigma Sagittarius A* (2003. 2 Tel.) - 11 sigma Linton, WatsonFest, Leeds July 2004

  26. HESS Galactic Center! Linton, WatsonFest, Leeds July 2004

  27. What is the Dark Matter? F. Zwicky Coma cluster

  28. HESS Galactic Center neutralino m > 10 TeV ??? Linton, WatsonFest, Leeds July 2004

  29. Many questions remain • What is the Dark Matter? • What is the Dark Energy? • What is the origin & max energy of cosmic rays? • Astro-Physics at high energy, curvature, and/or density? • What are the neutrino masses and underlying theory? • Why is there something rather than nothing? • Is there A Fundamental Theory? Quantum Gravity, Large Extra-Dimensions, Strings, M-theory,...? • How did the Universe Begin?

  30. Cosmological Constant Natural scale for : Contrast with: + coincidence…  ~M

  31. Many questions remain • What is the Dark Matter? • What is the Dark Energy? • What is the origin & max energy of cosmic rays? • Astro-Physics at high energy, curvature, and/or density? • What are the neutrino masses and underlying theory? • Why is there something rather than nothing? • Is there A Fundamental Theory? Quantum Gravity, Large Extra-Dimensions, Strings, M-theory,...? • How did the Universe Begin?

  32. Cosmic Rays • 1912 discovered by Victor Hess • (after Wilson & others) • Energy range: • ~ 109 eV to > 1020 eV • 1938Pierre Auger discovered • Extensive Air Showers (EAS) ORIGIN? Unknown! soon to be a Century Old Puzzle! at all energies…

  33. HESS 2 smoking guns CR acceleration! Galactic Centre - 11  RX J1713 - 20  Linton, WatsonFest, Leeds July 2004

  34. CRs at the Highest Energies Great Opportunity for Discovery can traverse longer distances than photons can point back to the source should have spectral features

  35. cosmic rays / / / / / / / / / / / n

  36. UHE proton trajectories in Extra Galactic B at the Highest Energies (1020 eV)) - should point to sources (unless Magnetic Fields are stronger &/or Z is larger) Isola, Lemoine, Sigl ‘02 lower bound 2 1019 eV to 3 1020eV, E-2.4 injection, BMpc ~0.3 G, Kolmog

  37. 6 doublets 1 triplet above 4 x 1019 eV < 2.5 deg AGASA above 1019 eV Log E>19.4 Log E>19.6

  38. HiRes HiRes-I Monocular Data, E > 1019.5 eV No clustering seen so far! HiRes-I Monocular Data, E > 1018.5 eV Upper limit of 4 doublets (90% c.l.) in HiRes-I monocular dataset. HiRes Stereo

  39. CRs at the Highest Energies can traverse longer distances than photons can point back to the source should have spectral features

  40. -resonance multi-pions High Energy Proton sees Cosmic Microwave Background as High Energy Gamma Rays! WMAP p+cmb +  p + 0  n +  + Proton Horizon GZK Cutoff Greisen ‘66, Zatsepin & Kuzmin ‘66

  41. GZK feature is source & B dependent… E. Parizot et al. ‘03

  42. AGASA High Energy Spectrum AGASA: ~ 11 events above 1020 eV!!!

  43. Comparisons 2003

  44. Two Spectra at High Energies

  45. Statistics Fluctuations at GZK feature are large for AGASA & HiRes 400 realizations of GZK feature for low statistics DeMarco, Blasi, & A.O. ‘03

  46. Auger (S) x AGASA DeMarco, Blasi, A.O. ‘03

  47. Pierre Auger Project • 2 Giant AirShower Arrays • South – Argentina Funded • North – Not Yet Funded • 1600 particle detectors over • 3000 km2 • + 4 Fluorescence Detectors • Will Measure Direction, • Energy, & Composition of • ~ 60 events/yr E > 1020eV • ~ 6000 events/yr E > 1019eV > 250 scientists from 16 countries Vietnam! J. Cronin and T. Yamamoto

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