1. The Revolution for the Rest of Us George Musser 6 October 2006

2. Zooming Out Source: Millennium Simulation (http://www.mpa-garching.mpg.de/galform/millennium/)

3. Zooming Out Source: Millennium Simulation (http://www.mpa-garching.mpg.de/galform/millennium/)

4. The (Very) Big Picture

5. Our Lineage

6. Cosmic Lineage

7. Expansion of Space

8. Thinning Out

9. Formation of Coherent Bodies

10. The “Revolution”

11. Four Pillars of Big Bang Theory 1.Galaxy recession (expansion of space) 2.Cosmic microwave background radiation 3.Abundance of light chemical elements 4.Arrangement of galaxies

12. Pillar #1: Expansion Rate Sources: Sandage, ApJ 307:1 (1986); de Vaucouleurs, PNAS 90:4811 (1993) Is It Slow?Or Fast? H 0 =55 km/s/MpcH 0 =86 km/s/Mpc

13. Source: Freedman et al. (astro-ph/0012376) Resolving the Dispute

14. Source: Freedman et al. (astro-ph/0012376) Resolving the Dispute

15. Past Expansion Rate

16. Source: Saul Perlmutter, Physics Today, April 2003 Past Expansion Rate

17. Decelerating

18. Accelerating

19. Pillar #2: Afterglow

20. Source: WMAP Science Team (http://map.gsfc.nasa.gov/m_or/mr_media2.html) COBE resolution Size of observable universe at 400,000 yr

21. Lots of Spots Source: http://space.mit.edu/home/tegmark/wmap3.html VentiGrandeTall

22. Pillar #3: Nucleosynthesis Source: 2006 Particle Data Book (http://pdg.lbl.gov/2006/reviews/bigbangnucrpp.pdf)

23. Pillar #4: Large-Scale Structure Adapted from Gott et al. (astro-ph/0310571)

24. Master Power Spectrum Source: Max Tegmark (http://space.mit.edu/home/tegmark/sdss.html)

25. Spots Reprise Source: Eisenstein et al., ApJ 633:560 (2005)

26. Concordance Model How much stuff is there? What kinds of stuff? What is it doing?

27. How Much Stuff? The Omega Problem Cluster 0024+1645 Theorists: Ω = 1Observers: Ω ~ 0.3 Source: http://hubblesite.org/newscenter/newsdesk/archive/releases/1996/10/image/a

28. Settling the Omega Dispute Source: Tegmark et al. (astro-ph/0608632)

29. What Kinds of Stuff? Source: Ostriker & Steinhardt, Sci Am Jan 2001

30. Radiation Era and Matter Era

31. Overall Composition Source: Ostriker & Steinhardt, Sci Am Jan 2001

32. Dark Matter Is Boring. Good! Time Radiation Era Matter Era Atoms form Dark matter Ordinary matter Adapted from slide by Seb Oliver (http://astronomy.sussex.ac.uk/~sjo/teach/dist2003/lecture19-lss/lecture19.ppt) Density contrast 60 kyr400 kyr

33. Without DM, Galaxies Are Toast Source: Max Tegmark (http://space.mit.edu/home/tegmark/movies_60dpi/fb_movie.html) 28% dark, 3% ordinary19%, 12% 16%, 16%0%, 30%

34. Source: Sean Carroll (http://cosmicvariance.com/wp-images/dmmotivator_01.jpg)

35. Overall Composition Source: Ostriker & Steinhardt, Sci Am Jan 2001

36. The Dark Energy Era

37. Cosmic Eras Radiation Era Matter Era Dark Energy Era

38. Cosmic Eras Inflation Era Radiation Era Matter Era Dark Energy Era

39. Structure Formation Source: Andrey Kravtsov  http://cosmicweb.uchicago.edu/filaments.html) Scale: 140 Mlyr

40. Summary So Far Precision observations Tidy end to old debates Dark energy given a catchy name But Is It Really a “Revolution”? Same model (big bang + inflation) Same theoretical basis (relativity) Same types of observations (pillars)

41. What’s the Cultural Impact? From Entretiens sur la pluralité des mondes, Bernard le Bovier de Fontenelle, 1686 From Annie Hall

42. Cosmology  Fundamental Physics Large Hadron Collider Mysteries The Great Big Particle Accelerator in the Sky

43. Cosmology  Fundamental Physics Mysteries The Great Big Particle Accelerator in the Sky The Great Big Microscope in the Sky

44. The Tree of Physics Simpler

45. Hierarchy of Scale aka The devil isn’t in the details.

46. Holographic Principle

47. Possibility vs. Actuality aka What can be, is. (Or is it?)

48. The Oddities of an Infinite (or Very Large) Space

49. What do the laws of physics require, and what do they simply allow? What is mandated, and what is happenstance? What does happenstance mean, anyway? If everything that is possible doesn’t happen, then what makes the choice?

50. Cosmic Coincidence You are here

51. The Best May Be Yet to Come! Whole new particle families (Large Hadron Collider) Evidence for extra dimensions (LHC) Signals from before the big bang (Planck satellite, gravitational-wave observatories) Evidence that spacetime is discrete (gamma-ray dispersion, interferometer fluctuations) Detection of dark matter (particle detectors) Tests of multiverse concept (galaxy observations, quantum unitarity experiments)

53. Bullet Cluster Slides

54. Bullet Cluster Source: http://chandra.harvard.edu/press/06_releases/press_082106.html Optical (galaxies)

55. Bullet Cluster Source: http://chandra.harvard.edu/press/06_releases/press_082106.html Optical (galaxies) X-Ray (gas)

56. Bullet Cluster Source: http://chandra.harvard.edu/press/06_releases/press_082106.html X-Ray (gas)

57. Bullet Cluster Source: http://chandra.harvard.edu/press/06_releases/press_082106.html X-Ray (gas) Lensing (mass)

58. Bullet Cluster Source: http://chandra.harvard.edu/press/06_releases/press_082106.html X-Ray (gas) Lensing (mass)

60. Old Expansion Slides

61. Sources: Freedman et al. (astro-ph/0012376) Current expansion rate

62. Sources: Freedman et al. (astro-ph/0012376) Current expansion rate

63. Sources: Freedman et al. (astro-ph/0002376  Ned Wright (http://www.astro.ucla.edu/~wright/sne_cosmology.html) Past expansion rateCurrent expansion rate Best fit