Cosmic Microwave Background Radiation (CMBR)

1. Cosmic Microwave Background Radiation (CMBR) • Relic of the Big Bang (“afterglow” of initial fireball) predicted in late 1940s • Discovered by Penzias & Wilson in 1965 — they won the Nobel Prize for this discovery • CMBR studied in detail by satellites (COBE, WMAP) • Radiation comes from era of decoupling of matterand radiation in the early Universe (~300,000 years old) when neutral H atoms first formed

2. Observations of the CMBR • CMBR very smooth — photons from different directions have the same properties • Earth’s motion with respect to the CMBR is detectable — one half of sky hotter by one part in 1000 • Satellite observations detected tiny fluctuations in CMBR (1 part in 100,000) that represent seeds of density fluctuations from which galaxies arose

3. i>clicker quiz #25 Which of the following statements isFALSE? • The Cosmic Microwave Background Radiation is considered to be strong evidence in favor of the Big Bang theory • The Steady State theory is founded on the Cosmological Principle • Most astronomers believe that the Universe satisfies the Cosmological Principle but not the Perfect Cosmological Principle • The Steady State theory postulates that, as the Universe expands, matter in the form of galaxies is created out of the energy in the C-field (“Creation” field)

4. Major Epochs in the Early Universe • t<3x105 years: Universe radiation dominated • t>3x105 years: Universe matter dominated • Why? • Let R be the scale length of the Universe (the separation between your favorite pair of galaxies, say). • Energy density of matter α 1/R3 since volume α R3 • Energy density of radiation α1/R4 since λ“stretched out”α R. By Wien's Law, T decreases as 1/R, and by the blackbody eqn. energy density decreases as T4α 1/R4

5. Unification of Forces • All four fundamental forces of Nature unified at t<10-43 s, the Planck time. • Gravity `froze' out separate from the other three forces at this time. • Next the strong nuclear force froze out at t=10-35 s • Weak and electromagnetic forces unified until t=10-12 s • Electroweak unification confirmed in the laboratory during the 1980s at CERN particle accelerator in Europe.

7. i>clicker quiz #26 Which of the following statements isFALSE? • Most of the mass in the Milky Way galaxy is thought to be in the form of non-luminous “dark matter” whose exact nature is unknown • Albert Einstein introduced the Cosmological constant Λ to obtain a static solution to the field equations of General Relativity because he believed at that time that the Universe was not expanding • Hubble’s law: v = H0d indicates that the Universe is expanding uniformly • Edwin Hubble discovered that the expansion rate of the Universe is speeding up because of a repulsive anti-gravity force associated with “dark energy”

8. Baryon Asymmetry • Extremely hot radiation in the few seconds after the Big Bang • Very energetic photons → continuous interchange of radiation into matter and vice versa (via pair production and pair annihilation). • Observable Universe is made up of mostly matter (as opposed to anti-matter) • Implies a slight asymmetry between matter and anti-matter in the very early Universe (a little more matter than antimatter) • This is referred to as the `baryon asymmetry' of the Universe

9. Confinement and Recombination • Quarks are the basic particles that protons and neutrons are thought to be composed of. • t=10-6 sec (T=1013 K), quarks were able to combine to form protons and neutrons → the epoch of confinement. • After t= 3x105 years the temperature dropped to T=3000 K • Protons and electrons (and neutrons) were able to combine to form neutral atoms. • Matter and radiation practically ceased to interact with each other (i.e., the Universe became transparent to radiation → CMBR). • The epoch of decoupling of matter and radiation or the epoch of recombination.

10. i>clicker quiz #27 Which of the following statements isFALSE? • Black holes emit Hawking radiation which can be characterized as thermal radiation and it is related to pair-production/annihilation from vacuum energy near the Schwarzschild radius or event horizon • The event horizon or Schwarzschild radius of a black hole, the region over which it is capable of trapping light (radiation), is proportional to the black hole’s mass • “A black hole has no hair” is a statement that describes the loss of identity of matter when it is swallowed by a black hole • The gravitational field of a black hole extends only out to its event horizon or Schwarzschild radius

12. Big Bang Nucleosynthesis • Almost all the hydrogen we see in the present Universe was formed at the epoch of recombination • Most of the light elements (helium, deuterium, lithium, etc.) were formed shortly thereafter • The efficiency with which these light elements were formed depends on what the density of protons and neutrons was (baryonic matter). • Studying the abundance of light elements (relative to hydrogen) is a good way of determining the baryon content of the Universe. • There is a fairly strong indication that most of the matter in the Universe is non-baryonic, in addition to being non-luminous.

13. The CMBR Horizon Problem • The CMBR has the same properties in all directions. • Consider two portions of the Universe from opposite ends of the sky. • These two portions are within our observable Universe (horizon), but they are outside each other's horizons. • Light has not yet had time to travel from one of these portions to the other. • If they have never been in communication, how do they know to be at the same temperature?

14. Inflation • Very early phase of extremely rapid expansion (Guth, Linde, 1980s). • During this inflationary phase, the Universe expands by a factor of 1050 in the time span t= 10-35 sec to t= 10-24 sec. • Inflationary phase is immediately after the epoch at which the strong nuclear force froze out, and before the weak nuclear force and electromagnetic force froze apart from each other. • All of our observable Universe was an infinitesimally small volume 1050x1050x1050= 10150 times smaller than we would have guessed from a simple extrapolation of the expansion we observe today.

15. Solving the Horizon Problem • Two parts of the Universe on opposite sides of the sky now outside each other's horizons. • Prior to inflationary epoch, these two patches would have been within each other's horizons and therefore `known' to acquire the same temperature. • Inflation caused them to expand out of each other's horizon. • Inflation requires the universe to expand faster than the speed of light. • Does not violate relativity — STR only applies in flat spacetime (i.e., in weak gravitational fields). • Special relativity is a special case of General relativity; inflation does obey the equations of General relativity.

16. Inflation, continued • Why is the density of the present Universe so close to critical (or why is the geometry of the observable Universe so close to flat)? • The scale of the observable Universe is much smaller than its `radius of curvature'. • What causes the rapid expansion during the inflationary era? • Inflation may be thought of as a phase transition in the Universe (as in a transition from a liquid to solid phase). • The `latent heat' in this phase transition builds up into an extremely high vacuum energy density, and this drives the expansion (analogous to the repulsive effect of Einstein's cosmological constant Λ).

17. i>clicker quiz #28 Which of the following statements isTRUE? • Most of the mass in the Milky Way galaxy is thought to be in the form of ordinary luminous stars • Albert Einstein introduced the Cosmological constant Λ to obtain a static solution to the field equations of General Relativity because he believed at that time that the Universe was not expanding • Hubble’s law: v = H0d indicates that the Universe’s expansion is accelerating • Edwin Hubble discovered that the expansion rate of the Universe is slowing down because of gravitational forces between galaxies

18. i>clicker quiz #29 Which of the following statements about the EPOCH OF CONFINEMENT is TRUE? • At this instant, quarks became bound in sets of three to produce protons and neutrons, while matter and radiation continued to interact strongly • The Universe was matter dominated at this epoch • Protons and electrons formed stable hydrogen atoms for the first time at this epoch, and the matter in the Universe became mostly transparent to radiation • This epoch was immediately followed by Inflation

19. i>clicker quiz #30 Which of the following statements isTRUE? • Inflation ended right at Planck time when the Universe was 10-50 seconds old • Gravity was the last of the four fundamental forces of Nature to “freeze” out (i.e. develop a unique identity) • Radiation dominated over matter at very early times in the Universe’s history, but matter has dominated over radiation ever since the Universe’s 300,000th birthday • Most of the elements in the periodic table that we learn about in school/college today were synthesized in the early Universe and this is known as Big Bang Nucleosynthesis

20. Solar system: 9 light hours diameter

21. Spiral galaxy: 80,000 light years diameter

22. Coma cluster of galaxies: 2.5 million light years across

23. Survey of distant galaxies: 5 to 9 billion light-years away

24. Cosmic Microwave Background Radiation (after-glow from the Big Bang) - edge of the observable Universe: 14 billion light years away

25. The Detailed Structure of a Spiral Galaxy

26. i>clicker quiz #31 Which of the following statements about INFLATION isFALSE? • The Universe expands faster than the speed of light during Inflation • The rapid expansion during Inflation naturally explains why spacetime appears to be “flat” in terms of its geometric properties • Inflation solves the CMBR horizon problem • Inflation violates the principles of Einstein’s General Theory of Relativity • The theory of Inflation predicted that there should be fluctuations at the level of 1 part in 105 in the CMBR

27. i>clicker quiz #32 Which of the following statements is FALSE? The Michelson-Morley experiment established that light is bent in a strong gravitational field Einstein received the Nobel Prize in Physics for explaining the photo-electric effect and the “particle” (photon) nature of light Kepler’s laws can be used to describe the motion of planets around the Sun Hubble is credited with the discovery of the expansion of the Universe Guth and Linde formulated the theory of Inflation

28. Introduction to Galaxies Basic Structure • How densely packed are stars in a galaxy?  Size (diameter) of a typical star: 106 km  Distance between stars: 1 pc = 3 x 1013 km  Analogy: 1 cm sized marbles separated by 300 km! • What fills in the space between stars?  Interstellar medium: gas, dust

29. Disk Galaxies: Structural Components • Flattened differentially-rotating disk • Dense centrally-concentrated bulge with mostly disordered orbits • Extended, not centrally concentrated, mostly dark halo • Bulge + Halo = “Spheroid”

31. Spiral Galaxy Properties • Bulge stars are older on average than disk stars • Youngest disk stars lie in very thin plane • Older disk stars lie in a thicker disk • Disk stars, particularly young ones, are organized into spiral arms • Spiral density waves in the disk: the most successful explanation of spiral structure

32. Globular Clusters

33. Globular Clusters • Most galaxies, including our own, contain dense clusters of 103– 106 stars known as globular clusters • The observed distribution of globular clusters tells us that the Sun is NOT at the center of the Milky Way galaxy

34. Galaxy Types • Spirals & irregulars (disk galaxies); ellipticals • Morphological (structural) features: Disk, bulge, bulge+disk, presence/absence of central bar • Nature of kinematics (internal motion of stars and gas): Coherent rotation of stars and gas in a disk; differential rotation Random motion of stars in the bulge of a spiral galaxy or elliptical

36. Hubble Sequence of Galaxies • Tuning fork diagram: E0-E7, S0 Sa-Sd / SBa-SBd, Irr • Morphological trends along the sequence: Shape (flattening) Bulge-to-disk ratio Spiral arms • Kinematical trends along the sequence: Ellipticals: mostly random motion, hardly any rotation Spirals: mostly rotation, hardly any random motion • Trends in the stellar mix: Ellipticals: mostly cool (old) stars Spirals: dominated by hot (young) stars