1. What is the Universe Made of? The Case for Dark Energy and Dark Matter Cliff Burgess

2. 1905 – A Big Year for Ann. Phys. Photo-electric Effect “On a Heuristic Point of View concerning the Production and Transformation of Light.” rcd Mar 18, pub Jun 9 Brownian Motion “On the Movement of Small Particles Suspended in Stationary Liquids Required by the Molecular-Kinetic Theory of Heat.” rcd May 11, pub Jul 18 Special Relativity “On the Electrodynamics of Moving Bodies.” rcd Jun 30, pub 26 Sep Size of Molecules* “A New Determination of Molecular Dimensions.” rcd Aug 19, pub Feb 8 Mass-Energy Equivalence “Does the Inertia of a Body Depend upon Its Energy Content?” rcd Sep 27, pub Nov 21 * PhD Thesis and most cited Albert Einstein

3. 1905 – A Big Year for Ann. Phys. Photo-electric Effect “On a Heuristic Point of View concerning the Production and Transformation of Light.” rcd Mar 18, pub Jun 9 Brownian Motion “On the Movement of Small Particles Suspended in Stationary Liquids Required by the Molecular-Kinetic Theory of Heat.” rcd May 11, pub Jul 18 Special Relativity “On the Electrodynamics of Moving Bodies.” rcd Jun 30, pub 26 Sep Size of Molecules* “A New Determination of Molecular Dimensions.” rcd Aug 19, pub Feb 8 Mass-Energy Equivalence “Does the Inertia of a Body Depend upon Its Energy Content?” rcd Sep 27, pub Nov 21 * PhD Thesis and most cited Albert Einstein

4. Outline The Hot Big Bang Evidence for a Hot Expanding Universe Dark Matter and Dark Energy Contact With Fundamental Physics Dark Matter Why Dark Energy is Harder Outlook

5. Visible Matter in the Universe “Only two things are infinite, the universe and human stupidity, and I’m not sure about the former.” Albert Einstein

6. Visible Matter in the Universe Visible matter is distributed as stars and gas within galaxies and clusters of galaxies. These appear to be distributed roughly isotropically and homogeneously about us. Courtesy: Jason Ware 2MASS Galaxy Survey

7. Courtesy: Sloan Digital Sky Survey WMAP A 3D View

8. Evidence for an Expanding Universe The sky is dark The Hubble Law The homogeneity and isotropy of the universe The slower decay of more distant supernovae In all directions galaxies are seen to be receding from us with a speed which is proportional to their distance from us: As expected if all started at the same point at the same instant.

9. Evidence for an Expanding Universe The sky is dark The Hubble Law The homogeneity and isotropy of the universe The slower decay of more distant supernovae Courtesy: Ned Wright’s Cosmology Page

10. Evidence for an Expanding Universe The sky is dark The Hubble Law The homogeneity and isotropy of the universe The slower decay of more distant supernovae Courtesy: Ned Wright’s Cosmology Page

11. Evidence for an Expanding Universe The sky is dark The Hubble Law The homogeneity and isotropy of the universe The slower decay of more distant supernovae Courtesy: Ned Wright’s Cosmology Page

12. The Hot Big Bang Matter in an expanding container cools. Extrapolating back in time suggests the Universe was once very small and very hot. The Hot Big Bang theory assumes the Universe was initially a small, hot soup of elementary particles. This theory is just now being redundantly tested. Surprise! Most of the matter in the Universe is in two completely unknown forms!

13. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance When the universe cools to the point where nuclei can form (around 10 10 K) then the relative abundances of the light elements can be calculated. The predictions for the isotopes of H, He, Li and Be agree with the measured abundances. Agreement is very sensitive to the total number of atoms present.

14. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999

15. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999 Total Mass Density of Atoms

16. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999 Total Mass Density of Atoms

17. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999 Total Mass Density of Atoms

18. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999 Total Mass Density of Atoms

19. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance Courtesy: Ned Wright’s Cosmology Page Burles, Nolette & Turner, 1999 Total Mass Density of Atoms

20. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance When the universe cools enough for atoms to form (around 10 3 K) it becomes transparent to light. The light present at this time is still running around the universe. This light is now seen as microwaves due to the intervening expansion of the universe.

21. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance

22. Evidence for a Hot Big Bang Primordial element abundances The cosmic microwave background T CMB vs distance COBE collaboration

23. Outline The Hot Big Bang Evidence for a Hot Expanding Universe Dark Matter and Dark Energy Contact With Fundamental Physics Dark Matter Why Dark Energy is Harder Outlook

24. Evidence for Dark Matter Mass in galaxies Mass in clusters of galaxies Temperature fluctuations in the CMB Start of galaxy formation.

25. Evidence for Dark Matter Mass in galaxies Mass in clusters of galaxies Temperature fluctuations in the CMB Start of galaxy formation.

26. Evidence for Dark Matter Mass in galaxies Mass in clusters of galaxies Temperature fluctuations in the CMB Start of galaxy formation. Courtesy: Ned Wright’s Cosmology Page

27. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Very distant objects should not precisely follow Hubble’s Law because gravitational attraction should decelerate the universal expansion. This can be tested by looking for deviations from Hubble’s Law for very distant supernovae.

28. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole

29. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page The universal expansion should be decelerating due to gravitational attraction Expect this:

30. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page Tonrey et.al., 2003

31. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page Tonrey et.al., 2003 Amount of Dark Energy Amount of Dark Matter

32. Evidence for Dark Energy WMAP collaboration Small temperature variations, at the level of one part in 100,000, are visible in the CMB Brightness of very distant supernovae Flatness of the universe as a whole

33. Evidence for Dark Energy WMAP collaboration These are due to sound waves in the primordial gas which emitted this light. Brightness of very distant supernovae Flatness of the universe as a whole

34. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page Size of the CMB fluctuations depends on the geometry of space the light traverses.

35. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page …but the geometry of space depends on the amount and kind of matter it contains

36. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page WMAP collaboration Measured H 0 with CMB fluctuations prefers a flat universe. Amount of Dark Matter Amount of Dark Energy

37. Evidence for Dark Energy Brightness of very distant supernovae Flatness of the universe as a whole Courtesy: Ned Wright’s Cosmology Page WMAP collaboration Dark Energy required to explain CMB is consistent with what universal acceleration requires. Amount of Dark Matter Amount of Dark Energy

38. Concordance Cosmology From best fits to the ‘Concordance Cosmology’ Courtesy: Ned Wright’s Cosmology Page

39. Outline The Hot Big Bang Evidence for a Hot Expanding Universe Dark Matter and Dark Energy Contact With Fundamental Physics Dark Matter Why Dark Energy is Harder Outlook

40. Contact With Fundamental Physics “If you are out to describe the truth, leave elegance to the tailor.” Albert Einstein

41. What is the Dark Matter? Ordinary atoms? Modifications to the Law of Gravity? New kind of particles?

42. What is the Dark Matter? Ordinary atoms? Modifications to the Law of Gravity? New kind of particles? Courtesy: Ned Wright’s Cosmology Page

43. What is the Dark Matter? Ordinary atoms? Modifications to the Law of Gravity? New kind of particles? The devil is in the details: No proposals yet succeed for galaxies and clusters and the CMB. Very difficult to modify gravity at long distances without having problems with fundamental principles.

44. What is the Dark Matter? Ordinary atoms? Modifications to the Law of Gravity? New kind of particles? Weakly Interacting Massive Particles arise in most theories of microscopic physics. Their residual cosmic abundance is naturally the right size to agree with the observed amount of Dark Matter.

45. Outline The Hot Big Bang Evidence for a Hot Expanding Universe Dark Matter and Dark Energy Contact With Fundamental Physics Dark Matter Why Dark Energy is Harder Outlook

46. What Cosmology Requires Small, positive energy density

47. What Cosmology Requires Small, positive energy density Negative pressure: p < -  /3 This expresses how the universal acceleration depends on the Dark Energy’s energy and pressure according to Einstein.

48. Vacuum Energy as Dark Energy The energy,, of the vacuum has the negative pressure required to be the Dark Energy. The vacuum energy is only observable through gravity because non gravitational measurements only see energy differences. log  log a

49. Vacuum Energy as Dark Energy If the vacuum can change slowly with time, so can the Dark Energy density. The condition : p < -  /3 requires the kinetic energy of the vacuum’s motion to be small at present. log  log aAlbrecht et.al., 2001

50. The Cosmological Constant Problem The vacuum energy is calculable within any theory of elementary particles, such as the Standard Model of particle physics. All elementary particles contribute quantum zero-point energy to the vacuum energy, Each particle of mass m contributes ≈ m 4 Since, for example, even the electron has m ~ 5 × 10 5 eV » 10 -3 eV, how can the vacuum have such a small energy density: « m 4 ?

51. Outlook “If I had only known, I’d have become a locksmith.” Albert Einstein

52. Outlook Cosmological observations are now redundantly testing the Hot Big Bang model. Observations support the ‘Concordance Cosmology’. The concordance involves several lines of independent evidence for both Dark Matter and Dark Energy. Neither can be dark forms of ordinary atoms. Dark Energy is difficult to embed into a fundamental theory, but a candidate now may exist which does so. If so, we’ll know from a variety of observational tests.

53. 1905 – 2005: A Centennial of Ideas “The most incomprehensible thing about the world is that it is at all comprehensible.” Albert Einstein