The Beginning of Time:

1. The Beginning of Time: Evidence for the Big Bang & the Theory of Inflation

3. A Brief History of the Universe • <10-43 seconds: Planck era • before the Planck time (all known laws of physics break down and we can’t say anything about what conditions were like) • 10-43 - 10-38 seconds: GUT era • all four forces are “unified” (have the same strength) • 10-38 -10-10 seconds: electroweak era • the electromagnetic and weak force become distinct.

5. the particle era • 10-10 - 0.001 seconds: particle era • plasma of fundamental particles (matter and anti-matter) • for some unknown reason, there must have been slightly more matter than anti-matter, at least in our corner of the Universe • at the end of the particle era, matter and anti-matter annihilate, leaving mostly matter. Photons outnumber protons by a billion to 1.

7. Big Bang Nucleosynthesis • 0.001 seconds– 3 minutes: nucleosynthesis temperatures of 109 K allow hydrogen nuclei to fuse into helium nuclei. proton deuterium 4He neutron 3H

8. the density of baryons • deuterium is formed in the course of fusing hydrogen to helium, and some is still left over • the observed ratio of deuterium to hydrogen and helium tells us the density of baryons (protons and neutrons) during the era of nucleosynthesis • observations of deuterium abundance show that the density of baryons is about 5 % of the critical density

9. prediction: hydrogen 75 % helium 25% • at very high temperatures (>1011 K) protons and neutrons can change into one another • as the Universe cools, protons (which are slightly less massive) become favored • ratio of protons to neutrons at the time when nucleosynthesis begins is predicted to be 7 to 1.

10. 3 minutes – 500,000 years: recombination hydrogen and helium nuclei capture electrons and become neutral atoms. The Universe becomes transparent to photons. Recombination

11. Stars and Galaxies • the plasma of neutral atoms gradually cools and protogalactic clouds form. • The first stars form out of the hydrogen and helium, make heavy elements, etc. • planets • life • astronomers • etc…

13. Light from the Big Bang • in 1965, Penzias and Wilson discovered an unexpected signal at microwave frequencies • this signal looked the same in all directions, and could not be attributed to any particular source • Penzias and Wilson thought there must be something wrong with their experiment!

14. Penzias & Wilson

15. Cosmic Microwave Background • it was soon realized that this radiation came from the hot Universe soon after the Big Bang! • cosmological redshifting over the huge distance this light has traveled has shifted the wavelength from the visible to the microwave

16. last scattering surface electrons attached to atoms, photons stream through electron plasma “soup” traps photons

17. COBE satellite

18. The COBE experiment • COBE showed that the CMB is an almost perfect blackbody (thermal) spectrum with a temperature of 2.73 K • the CMB is incredibly uniform in all directions; but COBE detected variations from place to place of one part in 105

19. Spectrum of the CMB

20. Temperature of the sky

21. Implications of COBE results: • the temperature and spectrum of the CMB measured by COBE is very strong confirmation of the hot Big Bang theory • the small temperature differences detected by COBE provide direct evidence that the Universe was lumpy on small scales at early times

22. The Boomerang experiment

24. Constraining the Geometry of the Universe

25. The MAP satellite

26. All sky temperature map: predicted results from MAP

27. in the next few years… • results from MAP and other new CMB experiments will allow us to determine the values of all of the cosmological parameters to an accuracy of 10 percent • matter density • geometry • baryon density • expansion rate (Hubble parameter) • and much more…

28. Some remaining questions • where did those lumps come from (needed to seed structure formation)? • why is the Universe so smooth on large scales? • why is the Universe so close to a flat geometry (implying that the density of matter and energy is very close to the critical density)?

29. Isotropy problem

31. Inflation • the theory of inflation is an attempt to solve all of these problems • this theory says that the Universe went through a brief period of very rapid expansion soon after the Big Bang – perhaps growing by as much as a factor of 1030 in 10-36 seconds. • perhaps caused by the “freeze out” of the strong force from the GUT “super-force”

32. The observable Universe

33. quantum fluctuations

34. Inflated quantum ripples • quantum fluctuations get expanded to the size needed to seed structure formation – and variations seen in the CMB

36. Inflation would have “expanded away” any curvature that the Universe may have once had

37. the flatness problem

38. We are here because, more than ten billion years ago, the Universe borrowed energy from the vacuum to create vast amounts of matter and anti-matter in nearly equal quantities…Your body is a collection of the atoms that were created billions of years ago in the interiors of stars, the fraction of a fraction of a percent of normal matter that escaped annihilation in the first microsecond of the Universe.