1. The Runaway Universe Dr Martin Hendry Dept of Physics and Astronomy University of Glasgow

2. Cosmology – the study of the Universe as a whole: Origin Evolution Eventual Fate

3. Cosmological theories depend on the available data

4. Ptolemy 90 – 168 AD Almagest (c 140 AD) Earth-Centred Universe

5. Nicolaus Copernicus 1473 – 1543 AD “In the true centre of everything resides the Sun” De Revolutionibus Orbis (1543)

6. Galileo Galilei: 1564 – 1642 AD

7. Galileo Galilei: 1564 – 1642 AD “I have observed the nature and the material of the Milky Way. With the aid of the telescope this has been scrutinized so directly and with such ocular certainty that all the disputes which have vexed philosophers through so many ages have been resolved, and we are at last freed from wordy debates about it. The galaxy is, in fact, nothing but a collection of innumerable stars grouped together in clusters. Upon whatever part of it the telescope is directed, a vast crowd of stars is immediately presented to view. Many of them are rather large and quite bright, while the number of smaller ones is quite beyond calculation.” from The Starry Messenger (1610)

8. Herschel’s Milky Way (1790)

9. The stars are VERY far away. The nearest star (after the Sun) is about 40 million million km from the Earth. It takes light more than 4 years to cross this distance (travelling at a speed of 300,000 km per second) If the Earth-Sun distance were the width of this screen, the nearest star would be in Rome !!!

10. Measuring Astronomical Distances: Parallax

11. Even the nearest star shows a parallax shift of only 1/2000 th the width of the full Moon

12. Brightness falls off with the square of the distance, because surface area of a sphere increases with the square of the radius Measuring Astronomical Distances: Inverse Square Law

13. Measuring Astronomical Distances: Inverse Square Law

14. Cepheid Variables: Cosmic Yardsticks Henrietta Leavitt 1908-1912

15. Herschel’s Milky Way (1790) Shapley’s Model (1915)

16. The nature of the nebulae?… Early 20 th Century Gas clouds within the Milky Way, or Island Universes?….

17. The Great Debate, 1920 Shapley vs Curtis at the National Academy of Sciences

18. The Great Debate, 1920 Shapley vs Curtis Shapley argues successfully that the nebulae are within the Milky Way at the National Academy of Sciences

19. 1922: Hubble finds Cepheids in the Great Nebula in Andromeda

20. Hubble measured distances to dozens of nearby nebulae Even the nearest, in Andromeda, was millions of light years distant

21. Hubble also measured the shift in colour, or wavelength, of the light from distant galaxies. Galaxy

22. Hubble also measured the shift in colour, or wavelength, of the light from distant galaxies. Galaxy Laboratory

23. Hubble also measured the shift in colour, or wavelength, of the light from distant galaxies. Galaxy Laboratory

24. Hubble’s Law: 1922 Distant galaxies are receding from us with a velocity proportional to their distance

25. ‘Recession of the Nebulae’ caused not by the motion of galaxies through space, but the expansion of space itself between the galaxies Hubble’s Interpretation

26. Einstein’s General Relativity “Matter tells spacetime how to curve, and spacetime tells matter how to move”

27. How fast is the Universe expanding? H0?H0?

28. Hubble’s Law V = H 0 d H 0 has units of (time) -1 – usually measured in kilometres per second per Megaparsec

29. Hubble’s Law V = H 0 d H 0 has units of (time) -1 – usually measured in kilometres per second per Megaparsec 1 pc = 3.26 light years = 3 10 16 m x

30. Hubble’s Law V = H 0 d H 0 has units of (time) -1 – usually measured in kilometres per second per Megaparsec 1 pc = 3.26 light years = 3 10 16 m x H 0 -1 = Hubble time = timescale for the expansion age of the Universe

31. Hubble’s Law V = H 0 d Hubble’s original work gave H 0 = 500 (in conflict with Geological timescale) ‘Modern’ values: dichotomy between H 0 = 50, and H 0 = 100 (with small statistical error) ????

32. Principal difficulty has been local distortions in ‘Hubble flow’ e.g. spectrum of M31 is blueshifted

33. Galaxies are clustered Structure in the Universe assembled by gravity

34. Galaxies are clustered Structure in the Universe assembled by gravity Locally, gravity sufficient to overcome cosmic expansion

35. Galaxies are clustered Structure in the Universe assembled by gravity Locally, gravity sufficient to overcome cosmic expansion On larger scales, expansion diluted: galaxies have peculiar velocity on top of Hubble velocity

36. Main local distortion due to Virgo cluster

37. Problem: Need to determine H 0 from remote galaxies, where peculiar motions are less important…. ….but…. We cannot use primary distance indicators to measure their distance Need Distance Ladder!!

39. HST Key Project, led by Wendy Freedman Measure Cepheid distances to ~30 nearby galaxies, Link Cepheids to Secondary distance indicators

40. HST has ‘bypassed’ one stage of the Distance Ladder, by observing Cepheids beyond the Local Group of galaxies

41. This has dramatically improved measurements of H 0

42. Virgo Cluster galaxy M100, 60 million light years distant…..

44. HST data also allows correction for the dimming effects of DUST

45. Must ensure that remote galaxy data are free from Selection Effects e.g. intrinsically brighter or bigger?…

46. Must ensure that remote galaxy data are free from Selection Effects e.g. intrinsically brighter or bigger?… Malmquist Bias

47. Must ensure that remote galaxy data are free from Selection Effects e.g. intrinsically brighter or bigger?… Malmquist Bias

48. Must ensure that remote galaxy data are free from Selection Effects e.g. intrinsically brighter or bigger?… Malmquist Bias H 0 = 70 7

49. Age of the Universe = 10 – 16 billion years (depends if the expansion is speeding up or slowing down)

50. Will the Universe continue to expand forever? To find out we need to compare the expansion rate now with the expansion rate in the distant past… Is the Universe speeding up or slowing down?

51. Answer depends on the geometry of the Universe

52. Einstein’s General Relativity “Matter tells spacetime how to curve, and spacetime tells matter how to move”

53. Answer depends on the geometry of the Universe Closed

54. Answer depends on the geometry of the Universe Closed Open

55. Answer depends on the geometry of the Universe Closed Open Flat

56. We can measure the geometry, and compare the expansion rate, using Supernovae….

57. Type Ia Supernova White dwarf star with a massive binary companion. Accretion pushes white dwarf over the Chandrasekhar limit, causing thermonuclear disruption Good standard candle because:- Narrow range of luminosities at maximum light Observable to very large distances

58. We can measure the geometry, and compare the expansion rate, using Supernovae….

59. Geometry of the Universe affects the relationship between distance and redshift of the supernovae Closed Open Flat

62. We can measure the geometry, and compare the expansion rate, using Supernovae…. ….and the Cosmic Background Radiation

63. Early Universe too hot for neutral atoms Free electrons scattered light (as in a fog) After 300,000 years, cool enough for atoms; fog clears!

64. Background radiation predicted in 1950s and 1960s by Gamov, Dicke, Peebles. Discovered in 1965 by Penzias and Wilson Arno Penzias and Robert Wilson Robert Dicke Jim Peebles

65. Cosmic Background Explorer (CoBE), launched 1989

66. CoBE map of temperature across the sky

68. CMBR ‘ripples’ are the seeds of today’s galaxies Galaxy formation is highly sensitive to the pattern, or power spectrum, of CMBR temperature ripples power spectrum

70. Position of first peak sensitive probe of the geometry of the Universe

71. Microwave Anisotropy Probe First WMAP results published February 2003

72. First year WMAP results published Tuesday 11 th Feb From Bennett et al (2003)

73. Position of first peak sensitive probe of the geometry of the Universe

74. Answer depends on the geometry of the Universe Closed Open Flat

75. Results: The expansion is accelerating The geometry of the Universe is FLAT The Universe will continue to expand indefinitely

76. Cosmological Constant? Quintessence? Dust?…. What is driving the cosmic acceleration?…

77. The future of the Universe:- No Big Crunch!!!