1. Concluding Comments For the Course Cosmology Fascinating Past Highly accomplished present (for example, the material covered in this course). Really exciting future

2. The History of the Universe Today Galaxy Formation Last Scattering Nuclear & High Energy Physics Inflation? Extra Dimensions? Time High Energy & Temp Anti-Gravity?*!

3. Concluding Comments For the Course Cosmology Fascinating Past Highly accomplished present (for example, the material covered in this course). Really exciting future

4. Past: Cosmology provided a great source of inspiration and new ideas:

5. Concluding Comments For the Course Cosmology Fascinating Past Highly accomplished present (for example, the material covered in this course). Really exciting future

6. Atomic energy levels Emission Absorption Present: Deep understanding of our universe comes from 1) Application of known laws of physics

7. Present: Deep understanding of our universe comes from 1) Application of known laws of physics

8. Present: Deep understanding of our universe comes from 2) Collecting amazing data sets

11. The Keck 10m Telescopes on Mauna Kea, Hawaii

12. Segments of the Keck 10m Telescope Mirror

16. 1996

17. Mass inferred from lensing: Must have dark matter

18. Present: Deep understanding of our universe comes from 3) Putting Data and physics together to get the big picture  Big Bang Theory

19. What we know about the big picture 1) On large scales the matter in the Universe is spread out very smoothly (“Homogeneous”) Mean density: 2) The Universe is expanding Hubble law:

20. The homogeneity of the Universe Isotropy of the microwave background (from the “edge of the observable universe”) to one part in 100,000 Galaxy

21. The homogeneity of the universe Galaxy surveys Radial Direction We are here

22. The homogeneity of the universe Galaxy surveys Radial Direction We are here From 1986

23. The Hubble law

24. The History of the Universe Today Galaxy Formation Last Scattering Nuclear & HEP Inflation? Extra Dimensions? Time High Energy & Temp Anti-Gravity?*!

25. Present: Deep understanding of our universe comes from 4) Exploring and observing consequences of the Big Bang such as CMB: The edge of the observable universe

26. The Edge of the Observable Universe: As we look back in space we look back in time. We see: Here & Now Light traveling from far away =from distant past Long ago (about 14 Billion years) the Universe was so hot and dense it was opaque: The edge of the observable universe

27. Today: Only 2.726K above absolute Zero “Microwave Radiation” (The “Cosmic Microwave Background”: CMB) 1,000,000 times weaker than ambient radiation in a pitch dark room. Properties of the Edge of the Observable Universe: Here & Now Similar to surface of Sun at time of emission

28. Today: Only 2.726K above absolute Zero “Microwave Radiation” (The “Cosmic Microwave Background”: CMB) 1,000,000 times weaker than ambient radiation in a pitch dark room. Properties of the Edge of the Observable Universe: Here & Now Similar to surface of Sun at time of emission Cools off due to cosmic expansion Same thing happens with stars “Oblers’ paradox” (see section 23.4)

29. Observing the Microwave Background, Past, present and future:

30. The History of the Universe Time High Energy & Temp New Image of the “Last Scattering Surface” from NASA’s WMAP satellite released Feb 11 2003

31. 2009 Updated after WMAP announce ment, Feb 2003 Real data Simulated data Real data ! 1993 Maps of the microwave sky (the “edge of the observable universe”

32. WMAP map of the “edge of the observable universe” plotted as a sphere

33. Note: we are really on the inside looking out

34. Present: Deep understanding of our universe comes from 4) Exploring and observing consequences of the Big Bang such as Formation of Nuclei

35. The History of the Universe Today Galaxy Formation Last Scattering Nuclear & High Energy Physics Inflation? Extra Dimensions? Time High Energy & Temp Anti-Gravity?*!

36. Present: Deep understanding of our universe comes from 5) New ideas such as cosmic inflation that seem to explain the start of the Big Bang and fit the data nicely

37. Characteristic oscillations in the CMB power Adapted from Bennett et al Feb 11 ‘03 WMAP “Active” models Inflation I.1 Successes Temperature Power   Angular scale

38. The future is exciting because of 1)Deep Mysteries  Dark Matter  Dark Energy

39. Cosmic acceleration (newest data) Using supernovae (exploding stars) as cosmic “mileposts”, acceleration of the Universe has been detected. Supernova Preferred by modern data  Amount of gravitating matter   Amount of “antigravity” matter  “Gravitating” non accelerating matter Here for inflation

40. Supernova Preferred by modern data  Amount of gravitating matter   Amount of “antigravity” matter  “Gravitating” non accelerating matter Here for inflation  Accelerating “Dark Energy” is what makes  U =1 (required to give consistency with inflation)  Acceleration or (required for inflation) is possible (+)  Dark Energy *very* poorly understood (-/+)

41. Dark Energy (accelerating) 70% Dark Matter 25% Ordinary Matter (observed in labs) 5% 95% of the cosmic matter/energy is a mystery. It has never been observed even in our best laboratories

42. The future is exciting because 2) Fantastic new data sets will enable us to explore these mysteries (and hopefully resolve some of them)

43. The future of cosmological data The James Webb (Next Generation) Space TelescopeThe James Webb (Next Generation) Space Telescope Proposed Launch Date: August 2011

44. Supernova Preferred by modern data  Amount of ordinary matter   Amount of “antigravity” matter  “Ordinary” non accelerating matter Here for inflation Proposed new experiment The SNAP Satellite

45. The future of cosmological data The LSST (Large-aperture Synoptic Survey Telescope) NB: the director of LSST is Prof Tony Tyson of UCD

46. The future of cosmological theory The new data will allow us to resolve hotly contested issues Expect progress on: Can we explain/understand the beginning of the universe? What is accelerating the universe? What caused the galaxies to form? What is the fundamental nature of matter and gravity?

47. For the future: -I hope this course has made you better able to understand new results as they are reported in the press. -Feel free to come around to my office hours at any time in the future with questions. - Perhaps some of you would like to make a career in cosmology research (feel free to see me & discuss that)