1. Cosmology

2. Observational evidence?

3. “Cosmologists are often in error but never in doubt.”
L.D. Landau

4. Cosmology
Observation #1: universe is homogeneous and isotropic at large scales
It cannot be stationary! It should expand or contract
Observation #2: universe is expanding (Hubble)
It should have a beginning!
Hot or cold??
Observation #3: Cosmic microwave background radiation
Hot Big Bang!

5. Fate of the universe: depends on mass distribution (or curvature)
Observation #4: Abundance of light elements
Confirms Hot Big Bang
Fate of the universe: depends on mass distribution (or curvature)
Observation #5: density measurements
Observation #6: Fluctuations of background radiation
Universe is nearly flat; it contains dark matter and “dark energy”

6. WHY our universe has the parameters that we observe?
Problems with standard Big Bang model
Theory of inflation
Formation of structure;
Planck scale,
Theory of Everything
WHY our universe has the parameters that we observe?
Anthropic Principle and beyond
"The Universe must have those properties which allow carbon-based life to develop within it at some stage in its history."

7. Observation #1: universe is very inhomogeneous and anisotropic at smaller scales …

8. Groups
clusters
superclusters

10. … but homogeneous and isotropic at large scale
(The Cosmological Principle)
The universe is homogeneous. This means there is no preferred observing position in the universe.
The universe is also isotropic. This means you see no difference in the structure of the universe as you look in different directions.

11. The Cosmological Principle
Considering the largest scales in the universe, we make the following fundamental assumptions:
1) Homogeneity: On the largest scales, the local universe has the same physical properties throughout the universe.
Every region has the same physical properties (mass density, expansion rate, visible vs. dark matter, etc.)
2) Isotropy: On the largest scales, the local universe looks the same in any direction that one observes.
You should see the same large-scale structure in any direction.
3) Universality: The laws of physics are the same everywhere in the universe.

13. The universe cannot be stationary!
Force per unit mass:
Energy per unit mass:

14. Conclusion: the universe should either contract or expand with decreasing speed, because the gravity slows down the expansion
What is in reality?

15. Hubble and Humason 1931: Vrecession = H0 R
The universe expands!
Edwin Hubble

16. Hubble’s Law
Distant galaxies are receding from us with a speed proportional to distance

17. The Necessity of a Big Bang
If galaxies are moving away from each other with a speed proportional to distance, there must have been a beginning, when everything was concentrated in one single point:
The Big Bang! ?

18. The Age of the Universe T ≈ d/v = 1/H ~ 15 billion years
Knowing the current rate of expansion of the universe, we can estimate the time it took for galaxies to move as far apart as they are today:
Time = distance / velocity
velocity = (Hubble constant) * distance
T ≈ d/v = 1/H ~ 15 billion years

19. Necessity of the Big Bang
Velocity = distance / time
The time of expansion is T ~ 1/H0 ~ 15 billion years
15 billion years ago all distances R were equal to 0
Current value of the Hubble constant H0  70 km/s/Mpc

20. Solution to Olbers’s Paradox:
Why is the sky dark at night?
If the universe is infinite, then every line of sight should end on the surface of a star at some point.
The night sky should be as bright as the surface of stars!
Solution to Olbers’s Paradox:
If the universe had a beginning, then we can only see light from galaxies that has had time to travel to us since the beginning of the universe.
The visible universe is finite!

21. Newtonian model of the universe
Mass within radius r(t):
Energy per unit mass:
Hubble law:

22. Hubble “constant” changes with time!

23. Main equation: Critical density: Solution for k = 0:
Indefinite expansion
Expansion will be replaced by contraction
Indefinite expansion but with speed approaching zero
Solution for k = 0:

24. But the age of globular clusters is 13 billion years!
Figure 15.12: If the behavior of the universe is determined by the density of matter and energy, then its fate is linked to its geometry. In these models, R is a measure of the extent to which the universe has expanded. Open-universe models expand without end, and the corresponding curves fall in the region shaded orange. Closed models expand and then contract back to a high-density state (red curve). Curves representing closed models fall in the region shaded blue. The dotted line represents a flat universe, the dividing line between open and closed models. Note that the estimated age of the universe depends on the rate at which the expansion is slowing down. (This figure assumes H = 70 km/s/Mpc.)
T = 2/3H0 = 9.5 billion years
But the age of globular clusters is 13 billion years!

25. Cosmology and General Relativity
According to the theory of general relativity, gravity is caused by
the curvature of space-time.
The effects of gravity on the largest cosmological scales should be related to the curvature of space-time!
The curvature of space-time, in turn, is determined by the distribution of mass and energy in the universe.
Space-time tells matter how to move;
matter tells space-time how to curve.

26. General relativistic models
Matter (mass, energy, pressure)
Einstein’s equations
Geometry of space-time

27. The Expanding Universe
On large scales, galaxies are moving apart, with velocity proportional to distance.
It’s not galaxies moving through space.
Space is expanding, carrying the galaxies along!
The galaxies themselves are not expanding!

28. 2D analogy with houses on the balloon

29. No center and no edge
Now add another dimension and you have our situation. Just like there is not new balloon material being created in the 2D analogy, new three-dimensional space is not being created in the expansion. Like any analogy, though, the balloon analogy has its limits. In the analogy, the balloon expands into the region around it---there is space beyond the balloon. However, with the expanding universe, space itself is expanding in three dimensions---the whole coordinate system is expanding. Our universe is NOT expanding ``into'' anything ``beyond''.

30. The Expanding Universe (2)
Hubble law does not mean that we are at the center of the universe!
You have the same impression from any other galaxy as well.

31. Expanding Space Analogy:
A loaf of raisin bread where the dough is rising and expanding, taking the raisins with it.

32. Raisin Bread
(SLIDESHOW MODE ONLY)

33. Cosmological redshift

34. General relativity picture
Galaxies are at rest in the comoving (expanding) frame
Due to the presence of matter, the universe is non-stationary: all distances change; scale factor R(t) is a function of time

35. Metric of the homogeneous and isotropic Universe
Robertson, Walker, Friedman, Lemaitre
Compare with metric for empty flat space:
Scale factor R(t) describes expansion or contraction
Curvature =

36. Finite, But Without Edge?
2-dimensional analogy: Surface of a sphere:
Surface is finite, but has no edge.
For a creature living on the sphere, having no sense of the third dimension, there’s no center (on the sphere!): All points are equal.
Alternative: Any point on the surface can be defined as the center of a coordinate system.

37. k = +1: positive curvature (sphere)
finite volume
k = -1: negative curvature (saddle)
k = 0: zero curvature (flat)
Curvature =

38. Shape and Geometry of the Universe
Back to our 2-dimensional analogy:
How can a 2-D creature investigate the geometry of the sphere?
Measure curvature of its space!
Flat surface
(zero curvature)
Closed surface
Open surface
(positive curvature)
(negative curvature)

39. p.309

40. p.309

41. p.309

42. Einstein’s equations:
Equation of state: relation between pressure P and energy density c2
 = 0 for dust (no pressure)
 = 1/3 for radiation (very hard pressure)
Or: acceleration =
Critical parameter

44. Hot or cold universe?? Microwave background radiation!
Any signatures of the past around us?
Microwave background radiation!
George Gamow (lived ) predicted in 1948 that there should be a faint glow left over from when the universe was much hotter and denser. The entire universe would have glowed first in the gamma ray band, then the X-ray band, then to less energetic bands as the universe expanded. By now, about 14 billion years after the start of the expansion, the cold universe should glow in the radio band.
Stopped here 12/1/05

45. George Gamow Born 1904 in Russia
Studied and worked at St.-Petersburg University
Fled Russia in 1934
Worked at GW University and University of Colorado
Proposed the concept of the Hot Big Bang
Explained the origin of chemical elements in the universe
Built the theory of radioactivity and explained the nucleosynthesis in stars
Proposed a concept of genetic code and explained how the code is implemented in DNA by the order of nucleotides
The cosmogenesis paper with Alpher (“The origin of chemical elements”) was published as the Alpher-Bethe-Gamow theory, Gamow had added the name of Hans Bethe to make a pun on the first three letters of the Greek alphabet, alpha beta gamma.

46. Looking Back Towards the Early Universe
The more distant the objects we observe, the further back into the past of the universe we are looking.

47. Figure 15.9: Photons scatter from electrons (black) easily but hardly at all from the much more massive protons (red). (a) When the universe was very dense and ionized, photons could not travel very far before they scattered off an electron. This made the gas opaque. (b) As the universe expanded, the electrons were spread further apart, and the photons could travel farther; this made the gas more transparent. (c) After recombination, most electrons were locked to protons to form neutral atoms, and the gas was highly transparent.
Fig. 15-9, p.304

48. The Cosmic Background Radiation
The radiation from the very early phase of the universe should still be detectable today
R. Wilson & A. Penzias
Was, in fact, discovered in mid-1960s as the Cosmic Microwave Background:
Blackbody radiation with a temperature of T = 2.73 K

49. Arno Penzias and Robert Wilson observed in 1965 a radio background source that was spread all over the universe---the cosmic microwave background radiation. The radiation has the same intensity and spectral character as a thermal continuous source at 3 K (more precisely, ± K) as measured by the COBE satellite in every direction observed. To a high degree of precision the sky is uniformly bright in radio. The uniformity of the background radiation is evidence for the cosmological principle.
From 3000 K to 2.7 K:
The redshift of 1000!

50. Figure 15.6: Three views of a small region of the universe centered on our galaxy. (c) Near us we see galaxies, but farther away we see young galaxies (dots), and at a great distance we see radiation (arrows) coming from the hot gas of the big bang.
Fig. 15-6c, p.301

51. The History of the Universe
Universe cools down as time passes
Universe expands as time passes

52. The Early History of the Universe
Electron
Positron
Gamma-ray photon
Electrons, positrons, and gamma-rays in equilibrium between pair production and annihilation

53. For reasons not completely understood, there was a very slight excess of ordinary matter over antimatter (by about 1 part in 109). This is why there was still some ordinary matter left over when all the antimatter had been annihilated. (This must be the case, otherwise you wouldn't be here!) All of the protons, neutrons, and electrons in matter today were created in the first few seconds after the Big Bang.

54. The Early History of the Universe (2)
25% of mass in helium 75% in hydrogen
Protons and neutrons form a few helium nuclei; the rest of protons remain as hydrogen nuclei
No stable nuclei with 5 and 8 protons
 Almost no elements heavier than helium are produced.

55. Cosmic Abundance of Helium and Hydrogen
The Big Bang theory provides a natural way to explain the present abundance of the elements. At about 2 to 3 minutes after the Big Bang, the expanding universe had cooled to below about 109 K so that protons and neutrons could fuse to make stable deuterium nuclei (a hydrogen isotope with one proton and one neutron) that would not be torn apart by energetic photons. Protons react to produce deuterium, deuterium nuclei react to make Helium-3 nuclei, and Helium-3 nuclei react to make the stable Helium-4 nucleus.
The deuterium nucleus is the weak link of the chain process, so the fusion chain reactions could not take place until the universe had cooled enough. The exact temperature depends sensitively on the density of the protons and neutrons at that time. Extremely small amounts of Lithium-7 were also produced during the early universe nucleosynthesis process. After about 15 minutes from the Big Bang, the universe had expanded and cooled so much that fusion was no longer possible. The composition of the universe was 10% helium and 90% hydrogen (or if you use the proportions by mass, then the proportions are 25% helium and 75% hydrogen).
Except for the extremely small amounts of the Lithium-7 produced in the early universe, the elements heavier than helium were produced in the cores of stars.

56. Figure 15. 8: Cosmic element building
Figure 15.8: Cosmic element building. During the first few minutes of the big bang, temperatures and densities were high, and nuclear reactions built heavier elements. Because there are no stable nuclei with atomic weights of 5 or 8, the process built very few atoms heavier than helium.
Fig. 15-8, p.303

57. Figure 15.14: This graph plots the abundance of deuterium and lithium-7 versus the present density of the universe. Observations of the abundance of deuterium and lithium-7 are uncertain, but they limit the density of normal matter in the universe to a narrow range (green bar). The density of normal matter cannot be more than 5 percent of the critical density ρo.
Fig , p.311

58. The Nature of Dark Matter
Can dark matter be composed of normal matter?
If so, then its mass would mostly come from protons and neutrons = baryons
The density of baryons right after the big bang leaves a unique imprint in the abundances of deuterium and lithium.
Density of baryonic matter is only ~ 4 % of critical density.
Most dark matter must be non-baryonic!

59. The Early History of the Universe (3)
Photons have a blackbody spectrum at the same temperature as matter.
Photons are incessantly scattered by free electrons; photons are in equilibrium with matter
Radiation dominated era

60. Transition to matter dominated era
Recombination
Protons and electrons recombine to form atoms => universe becomes transparent for photons
z ≈1000
Transition to matter dominated era

61. The Cosmic Background Radiation (2)
After recombination, photons can travel freely through space.
Their wavelength is only stretched (red shifted) by cosmic expansion.
Recombination:
z = 1000; T = 3000 K
This is what we can observe today as the cosmic background radiation!

62. Observations are consistent with Hot Big Bang Model
The cosmic microwave background radiation can be explained only by the Big Bang theory. The background radiation is the relic of an early hot universe. The Big Bang theory's major competitor, called the Steady State theory, could not explain the background radiation, and so fell into disfavor.
The amount of activity (active galaxies, quasars, collisions) was greater in the past than now. This shows that the universe does evolve (change) with time. The Steady State theory says that the universe should remain the same with time, so once again, it does not work.
The number of quasars drops off for very large redshifts (redshifts greater than about 50% of the speed of light). The Hubble Law says that these are for large look-back times. This observation is taken to mean that the universe was not old enough to produce quasars at those large redshifts. The universe did have a beginning.
The abundance of hydrogen, helium, deuterium, lithium agrees with that predicted by the Big Bang theory. The abundances are checked from the spectra of the the oldest stars and gas clouds which are made from unprocessed, primitive material. They have the predicted relative abundances.

63. Depends on mass-energy density (Curvature of Space)
Fate of the Universe
Depends on mass-energy density (Curvature of Space)
The more mass there is, the more gravity there is to slow down the expansion. Is there enough gravity to halt the expansion and recollapse the universe or not? If there is enough matter (gravity) to recollapse the universe, the universe is ``closed''. In the examples of curved space above, a closed universe would be shaped like a four-dimensional sphere (finite, but unbounded). Space curves back on itself and time has a beginning and an end. If there is not enough matter, the universe will keep expanding forever. Such a universe is ``open''. In the examples of curved space, an open universe would be shaped like a four-dimensional saddle (infinite and unbounded). Space curves away from itself and time has no end.

64. Deceleration of the Universe
Expansion of the universe should be slowed down by mutual gravitational attraction of the galaxies.
Fate of the universe depends on the matter density in the universe.
Define “critical density”, rc, which is just enough to slow the cosmic expansion to a halt at infinity.

65. Main equation: Critical density: Solution for k = 0:
Indefinite expansion
Expansion will be replaced by contraction
Indefinite expansion but with speed approaching zero
Solution for k = 0:

66. Model Universes
r < rc => universe will expand forever
Maximum age of the universe:
~ 1/H0
r = rc => Flat Universe
Size scale of the Universe
r > rc => Universe will collapse back
Time
If the density of matter equaled the critical density, then the curvature of space-time by the matter would be just sufficient to make the geometry of the universe flat!

67. Deriving geometry of the universe from density measurements

68. Orbital speeds of stars in galaxies

69. Faint gas shells around ellipticals
Ellipticals have faint gas shells that need massive ``dark'' haloes to contain them. The gas particles are moving too quickly (they are too hot) for the gravity of the visible matter to hang onto it.
Motion of galaxies in a cluster
Galaxy cluster members are moving too fast to be gravitationally bound unless there is unseen mass.
Hot gas in clusters
The existence of HOT (i.e., fast moving) gas in galaxy clusters. To keep the gas bound to the cluster, there needs to be extra unseen mass.
Quasar spectra
Absorption lines from hydrogen in quasar spectra tells us that there is a lot of material between us and the quasars.
Gravitational Lensing
Gravitational lensing of the light from distant galaxies and quasars by closer galaxies or galaxy clusters enables us to calculate the amount of mass in the closer galaxy or galaxy cluster from the amount of bending of the light. The derived mass is greater than the amount of mass in the visible matter.
Current tallies of the total mass of the universe (visible and dark matter) indicate that all matter constitutes only 27% of the critical density.

70. Deriving geometry of the universe from microwave background radiation

71. Cosmology with the Cosmic Microwave Background
If the universe were perfectly homogeneous on all scales at the time of recombination (z = 1000), then the CMB should be perfectly isotropic over the sky.
Instead, it shows small-scale fluctuations:

72. Evidence for the formation of galaxies and large-scale structure
Fluctuations of the CMB temperature
The universe could not have been perfectly uniform, though. The universe must have been slightly lumpy to form galaxies later on from the internal gravity of the lumps. Initial density variations had to exist in order to provide some direction to where surrounding matter could be attracted. The COBE satellite found slight variations in the brightness of the background radiation of about 1 part in 100,000. The slight variations exist because some parts of the universe were slightly denser than other parts. The slightly denser regions had more gravity and attracted more material to them while the expansion occurred. Over time, the denser regions got even denser and eventually formed galaxies about 1 billion years after the Big Bang.

73. CMB fluctuations are the direct probe of the Large Scale Structure
A large survey of distant galaxies shows the largest structures in the universe:
Filaments and walls of galaxy superclusters, and
voids, basically empty space.

76. Deriving geometry of the universe from microwave background radiation

77. The case of a missing Universe
Observations suggest that the universe is flat:  = 1
Visible matter accounts for ~ 4% of the total mass-energy density: v = 0.04
Dark matter accounts for only 27% of the total mass-energy density: DM = 0.27
The rest 70% is something else!!
This something else is termed “dark energy”
It apparently causes the universe to accelerate in its expansion!!

78. The accelerating Universe
distance
redshift z
or recession velocity

83. Figure 15.17: (a) A type Ia supernova erupts in a very distant galaxy and begins to fade. By calibrating these supernovae, astronomers were able to find the distances to some of the farthest visible galaxies. (ESO)

86. Supernovae are too faint
Figure 15.17: (b) Type Ia supernovae in distant galaxies are about 25 percent too faint, which must mean the galaxies are farther away from us than they would be in a universe expanding at a constant rate. This diagram shows observations of supernovae compared with a decelerating flat universe dominated by dark matter (blue line). The red line shows the relationship for an accelerating flat universe.

91. Einstein’s equations:
Equation of state: relation between pressure P and energy density c2
 = 0 for dust (no pressure)
 = 1/3 for radiation (very hard pressure)
Or: acceleration =
To have acceleration,
we must have negative pressure!
 = -1 ??

93. Accelerating now, but decelerating in the past?!

95. Figure 15.18: In a 1997 follow-up image of the Hubble Deep Field made in 1995, astronomers noticed a faint galaxy that was brighter in the second image (lower left). Subtracting the earlier image from the later image revealed a supernova cataloged as SN1997ff (lower right). The unexpected faintness of the supernova confirms that the universe is accelerating. (Adam Riess, STScI/NASA)
Fig , p.316

98. Problems with standard model. Inflation
Flatness problem
Horizon problem
Initial fluctuations
Absence of magnetic monopoles
“Fine tuning”

103. Solution of the Problems of the Big Bang by Inflation
If this inflationary epoch really took place, it could cure all the problems of the big bang:
The tremendous expansion means that regions that we see widely separated in the sky now at the horizon were much closer together before inflation and thus could have been in contact by light signals.
The tremendous expansion greatly dilutes any initial curvature. In fact, the inflationary theory predicts unequivocally that the Universe should globally be exactly flat, and therefore that the average density of the Universe should be exactly equal to the closure density.
The rapid expansion of the Universe tremendously dilutes the concentration of any magnetic monopoles that are produced. Simple calculations indicate that they become so rare in any given volume of space that we would be very unlikely to ever encounter one in an experiment designed to search for them.
Density Fluctuations as Seeds for Galaxy Formation
Detailed considerations indicate that inflation is capable of producing small density fluctuations that can later in the history of the Universe provide the seeds to cause matter to begin to clump together to form the galaxies and other observed structure.

104. What could be the reason for inflation?
Figure 15.16: When the universe was very young and hot (top), the four forces of nature were indistinguishable. As the universe began to expand and cool, the forces separated and triggered a sudden inflation in the size of the universe.
Fig , p.313

107. Do we live in a special universe??
Change of physical constants by a very small amount would
render impossible the life in the universe as we know it
Adding or subtracting just one spatial dimension would make
the formation of planets and atoms impossible
Life as we know it needs a universe which is large enough, flat,
homogeneous, and isotropic

108. Anthropic Principle
We observe the universe to be as it is because only in such a universe could observers like ourselves exist.
That is, selection effects would say that it is only in universes where the conditions are right for life (thus pre-selecting certain universe) is it possible for the questions of specialness to be posed.
This is a solution, but can we do better?

109. Our local country is nothing special (ancient travelers)
History of science teaches us that there is nothing special in the place we live
Our local country is nothing special (ancient travelers)
Planet Earth is nothing special (Copernicus)
Milky Way galaxy is nothing special (Hubble)
Our part of the Universe is nothing special
Self-reproducing Universe
Eternal Big Bang and ensemble of universes
Linde, Vilenkin

110. Landscape of the multiverse
Planck scale:
Planck Length
Planck Mass
Planck density 1094 g/cm3
Eternal multiverse;
Individual universes are being continuously “inflated” from a space-time “foam”.
Some of these universities can harbor life as we know it; others don’t.
A large fraction of universes CAN harbor life