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Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoints Slide Show mode (presentation mode)
содержание презентации «Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoints Slide Show mode (presentation mode).ppt»| Сл | Текст | Сл | Текст |
| 1 | Note that the following lectures | 34 | Superclusters appear aligned along walls |
| include animations and PowerPoint effects | and filaments. Vast regions of space are | ||
| such as fly ins and transitions that | completely empty: “voids”. | ||
| require you to be in PowerPoint's Slide | 35 | The Farthest Galaxies. The most | |
| Show mode (presentation mode). | distant galaxies visible by HST are seen | ||
| 2 | Chapter 16. Galaxies. | at a time when the universe was only ~ 1 | |
| 3 | Guidepost. The preceding chapter was | billion years old. | |
| about our Milky Way Galaxy, an important | 36 | New Terms. spiral nebula island | |
| object to us but only one of the many | universe Shapley–Curtis Debate elliptical | ||
| billions of galaxies visible in the sky. | galaxy spiral galaxy barred spiral galaxy | ||
| We can no more understand galaxies by | irregular galaxy megaparsec (Mpc) distance | ||
| understanding a single example, the Milky | indicator standard candle distance scale | ||
| Way, than we could understand humanity by | look-back time Hubble law Hubble constant | ||
| understanding a single person. This | (H) rotation curve rotation curve method | ||
| chapter expands our horizon to discuss the | cluster method. velocity dispersion method | ||
| different kinds of galaxies and their | rich cluster poor cluster ring galaxy | ||
| complex histories. We take two lessons | galactic cannibalism ultraluminous | ||
| from this chapter. First, galaxies are not | infrared galaxy starburst galaxy. | ||
| solitary beasts; they collide and interact | 37 | Discussion Questions. 1. From what you | |
| with each other. Second, most of the | know about star formation and the | ||
| matter in the universe is invisible. The | evolution of galaxies, do you think the | ||
| galaxies we see are only the tip of a | Infrared Astronomy Satellite should have | ||
| cosmic iceberg. We will carry the lessons | found irregular galaxies to be bright or | ||
| of this chapter into the next, where we | faint in the infrared? Why or why not? | ||
| will discuss violently active galaxies, | What about starburst galaxies? What about | ||
| and on into Chapter 18, where we discuss | elliptical galaxies? 2. Imagine that we | ||
| the universe as a whole. | could observe a gas cloud at such a high | ||
| 4 | Outline. I. The Family of Galaxies A. | look-back time that it is just beginning | |
| The Discovery of Galaxies B. The Shapes of | to form one of the first galaxies. | ||
| Galaxies C. How Many Galaxies? II. | Further, suppose we discovered that the | ||
| Measuring the Properties of Galaxies A. | gas was metal rich. Would that support or | ||
| Distance B. The Hubble Law C. Diameter and | contradict our understanding of galaxy | ||
| Luminosity D. Mass E. Supermassive Black | formation? | ||
| Holes in Galaxies F. Dark Matter in | 38 | Quiz Questions. 1. How was William | |
| Galaxies. | Parsons (Lord Rosse) in 1845 able to see | ||
| 5 | Outline (continued). III. The | spiral structure in some nebulae, whereas | |
| Evolution of Galaxies A. Clusters of | others had not noticed this spiral | ||
| Galaxies B. Colliding Galaxies C. The | structure before? a. He had incredibly | ||
| Origin and Evolution of Galaxies D. The | large pupils and keen eyesight. b. His | ||
| Farthest Galaxies. | observatory was located on a high, dry | ||
| 6 | Galaxies. Star systems like our Milky | mountain peak. c. His telescope, with a | |
| Way. Contain a few thousand to tens of | diameter of 72 inches, was the largest in | ||
| billions of stars. Large variety of shapes | the world. d. No nebulae had been observed | ||
| and sizes. | with a telescope before his time. e. His | ||
| 7 | Galaxy Diversity. Even seemingly empty | long time exposure photographs that | |
| regions of the sky contain thousands of | revealed the spiral structure. | ||
| very faint, very distant galaxies. | 39 | Quiz Questions. 2. What did William | |
| Spirals. Ellipticals. Irregular (some | Parsons (Lord Rosse) think the spiral | ||
| interacting). The Hubble Deep Field: | nebulae were? a. Spiral clusters of low | ||
| 10-day exposure on an apparently empty | luminosity stars located nearby. b. New | ||
| field in the sky. Large variety of galaxy | planetary systems in the process of | ||
| morphologies: | formation. c. Spiral star clusters located | ||
| 8 | Galaxy Classification. E0, …, E7. Sa. | in the Milky Way. d. Dying high-mass | |
| Large nucleus; tightly wound arms. E0 = | stars. e. Island universes. | ||
| Spherical. E1. Sb. Sc. Small nucleus; | 40 | Quiz Questions. 3. What was the topic | |
| loosely wound arms. E7 = Highly | of the Shapley-Curtis Debate of 1920? a. | ||
| elliptical. E6. | The location of the spiral nebulae. b. The | ||
| 9 | Gas and Dust in Galaxies. Spirals are | size of the Milky Way Galaxy. c. The | |
| rich in gas and dust. Ellipticals are | period-luminosity relationship of Cepheid | ||
| almost devoid of gas and dust. Galaxies | variable stars. d. The period-luminosity | ||
| with disk and bulge, but no dust are | relationship of RR Lyrae variable stars. | ||
| termed S0. | e. The time-sharing schedule of the new | ||
| 10 | Barred Spirals. Some spirals show a | 100 inch diameter telescope. | |
| pronounced bar structure in the center. | 41 | Quiz Questions. 4. Edwin Hubble | |
| They are termed barred spiral galaxies. | resolved the Shapley-Curtis debate in 1924 | ||
| Sequence: SBa, …, SBc, analogous to | by measuring the distance to large, bright | ||
| regular spirals. | spiral nebulae. What distance method did | ||
| 11 | Irregular Galaxies. Often: result of | Hubble employ? a. The parallax method. b. | |
| galaxy collisions / mergers. Often: Very | The Hubble Law method. c. The Cepheid | ||
| active star formation (“Starburst | variable star method. d. The spectroscopic | ||
| galaxies”). The Cocoon Galaxy. NGC | parallax method. e. The RR Lyrae variable | ||
| 4038/4039. Some: Small (“dwarf galaxies”) | star method. | ||
| satellites of larger galaxies (e.g., | 42 | Quiz Questions. 5. Galaxies with | |
| Magellanic Clouds). Large Magellanic | active star formation also have which of | ||
| Cloud. | the following? a. Plenty of gas and dust. | ||
| 12 | Galaxy Types. (SLIDESHOW MODE ONLY). | b. O and B associations. c. Emission | |
| 13 | Distance Measurements to Other | nebulae d. A bluish tint. e. All of the | |
| Galaxies (1). Cepheid Method: Using Period | above. | ||
| – Luminosity relation for classical | 43 | Quiz Questions. 6. The Hubble deep | |
| Cepheids: Measure Cepheid’s Period ? Find | field image reveals more than 1500 distant | ||
| its luminosity ? Compare to apparent | galaxies in a region about 1 arc minute in | ||
| magnitude ? Find its distance. b) Type Ia | diameter. If this density of galaxies is | ||
| Supernovae (collapse of an accreting white | typical over the whole sky, how many | ||
| dwarf in a binary system): Type Ia | distant galaxies are hidden from view at | ||
| Supernovae have well known standard | one instant by the Moon, with an angular | ||
| luminosities ? Compare to apparent | diameter of about 30 arc minutes? a. | ||
| magnitudes ? Find its distances. Both are | Approximately 150 distant galaxies are | ||
| “Standard-candle” methods: Know absolute | hidden behind the Moon at any given time. | ||
| magnitude (luminosity) ? compare to | b. Approximately 1500 distant galaxies are | ||
| apparent magnitude ? find distance. | hidden behind the Moon at any given time. | ||
| 14 | Cepheid Distance Measurement. Repeated | c. Approximately 15,000 distant galaxies | |
| brightness measurements of a Cepheid allow | are hidden behind the Moon at any given | ||
| the determination of the period and thus | time. d. Approximately 150,000 distant | ||
| the absolute magnitude. ? Distance. | galaxies are hidden behind the Moon at any | ||
| 15 | The Most Distant Galaxies. At very | given time. e. More than 1,000,000 distant | |
| large distances, only the general | galaxies are hidden behind the Moon at any | ||
| characteristics of galaxies can be used to | given time. | ||
| estimate their luminosities ? distances. | 44 | Quiz Questions. 7. How does a Sa | |
| Cluster of galaxies at ~ 4 to 6 billion | galaxy differ from a Sc galaxy? a. The Sa | ||
| light years. | galaxy has a smaller nuclear bulge. b. The | ||
| 16 | Distance Measurements to Other | Sa galaxy has more loosely wound spiral | |
| Galaxies (2): The Hubble Law. vr = H0*d. | arms. c. The Sa galaxy has less gas and | ||
| Measure vr through the Doppler effect ? | dust. d. Both a and c above. e. Both b and | ||
| infer the distance. E. Hubble (1913): | c above. | ||
| Distant galaxies are moving away from our | 45 | Quiz Questions. 8. What gives | |
| Milky Way, with a recession velocity, vr, | elliptical galaxies a redder color than | ||
| proportional to their distance d: H0 ? 70 | spiral galaxies? a. Elliptical galaxies | ||
| km/s/Mpc is the Hubble constant. | are more massive, and thus have a larger | ||
| 17 | The Extragalactic Distance Scale. Many | gravitational red shift. b. Elliptical | |
| galaxies are typically millions or | galaxies are more distant, and thus have | ||
| billions of parsecs from our galaxy. | more interstellar reddening. c. Elliptical | ||
| Typical distance units: Mpc = Megaparsec = | galaxies are more distant, and thus have | ||
| 1 million parsec Gpc = Gigaparsec = 1 | larger red shifts. d. Elliptical galaxies | ||
| billion parsec. Distances of Mpc or even | have a higher percentage of iron. e. | ||
| Gpc ? The light we see left the galaxy | Elliptical galaxies have less gas and | ||
| millions or billions of years ago!! | dust. | ||
| “Look-back times” of millions or billions | 46 | Quiz Questions. 9. What must we know | |
| of years. | about an object to use it as a distance | ||
| 18 | Galaxy Sizes and Luminosities. Vastly | indicator? a. The object’s luminosity. b. | |
| different sizes and luminosities: From | The object’s linear size. c. The object’s | ||
| small, low-luminosity irregular galaxies | age. d. Either a or b above. e. Either a, | ||
| (much smaller and less luminous than the | b, or c above. | ||
| Milky Way) to giant ellipticals and large | 47 | Quiz Questions. 10. Which of the | |
| spirals, a few times the Milky Way’s size | following is NOT a distance indicator used | ||
| and luminosity. | in galactic astronomy? a. White dwarfs. b. | ||
| 19 | Rotation Curves of Galaxies. Observe | Cepheid variable stars. c. Planetary | |
| frequency of spectral lines across a | nebulae. d. Type Ia supernovae. e. | ||
| galaxy. From blue / red shift of spectral | Brightest globular cluster. | ||
| lines across the galaxy ? infer rotational | 48 | Quiz Questions. 11. What observable | |
| velocity. Plot of rotational velocity vs. | property of a standard candle must be | ||
| distance from the center of the galaxy: | measured to determine its distance? a. | ||
| Rotation Curve. | Age. b. Mass. c. Luminosity. d. Angular | ||
| 20 | Determining the Masses of Galaxies. | size. e. Apparent magnitude. | |
| masses of galaxies. Based on rotation | 49 | Quiz Questions. 12. Why is a supernova | |
| curves, use Kepler’s 3rd law to infer. | type Ia standard candle better to use in | ||
| 21 | Masses and Other Properties of | measuring very long distances than either | |
| Galaxies. | the brightest globular cluster or Cepheid | ||
| 22 | Supermassive Black Holes. ? | variable star standard candles? a. Type Ia | |
| Supermassive black holes. From the | supernovae are more luminous. b. Globular | ||
| measurement of stellar velocities near the | star clusters and Cepheid variables exist | ||
| center of a galaxy: Infer mass in the very | only in the Milky Way Galaxy. c. Type Ia | ||
| center ? central black holes! Several | supernovae are very common. d. The | ||
| million, up to more than a billion solar | calibration of Type Ia supernovae is more | ||
| masses! | precise. e. Both c and d above. | ||
| 23 | Dark Matter. Adding “visible” mass in: | 50 | Quiz Questions. 13. When viewing a |
| stars, interstellar gas, dust, …etc., we | distant galaxy, the amount of look-back | ||
| find that most of the mass is “invisible”! | time in years is equal to the a. distance | ||
| The nature of this “dark matter” is not | to the galaxy in light years. b. | ||
| understood at this time. Some ideas: brown | round-trip distance to the galaxy in light | ||
| dwarfs, small black holes, exotic | years. c. time that has passed since the | ||
| elementary particles. | galaxy was first discovered. d. exposure | ||
| 24 | Clusters of Galaxies. Galaxies | time of a photograph that is taken of that | |
| generally do not exist in isolation, but | galaxy. e. time since you last looked at | ||
| form larger clusters of galaxies. Rich | the galaxy. | ||
| clusters: 1,000 or more galaxies, diameter | 51 | Quiz Questions. 14. What is the | |
| of ~ 3 Mpc, condensed around a large, | distance to a galaxy that has a | ||
| central galaxy. Poor clusters: Less than | recessional speed of 3500 km/s if the | ||
| 1,000 galaxies (often just a few), | Hubble constant is 70 km/s/Mpc? a. 10 Mpc. | ||
| diameter of a few Mpc, generally not | b. 20 Mpc. c. 30 Mpc. d. 40 Mpc. e. 50 | ||
| condensed towards the center. | Mpc. | ||
| 25 | Hot Gas in Clusters of Galaxies. Space | 52 | Quiz Questions. 15. What parameter |
| between galaxies is not empty, but filled | must we know to determine the linear | ||
| with hot gas (observable in X-rays). That | diameter and luminosity of a particular | ||
| this gas remains gravitationally bound | galaxy? a. The type of galaxy. b. The age | ||
| provides further evidence for dark matter. | of the galaxy. c. The mass of the galaxy. | ||
| Visible light. X-rays. Coma Cluster of | d. The distance to the galaxy. e. The | ||
| Galaxies. | amount of gas and dust in the galaxy. | ||
| 26 | Our Galaxy Cluster: The Local Group. | 53 | Quiz Questions. 16. Which type of |
| Milky Way. Andromeda galaxy. Small | galaxy has the largest range in both size | ||
| Magellanic Cloud. Large Magellanic Cloud. | and mass? a. Spiral. b. Elliptical c. | ||
| 27 | Neighboring Galaxies. Some galaxies of | Irregular. d. Both a and b have the same | |
| our local group are difficult to observe | range. e. All of the above have the same | ||
| because they are located behind the center | range. | ||
| of our Milky Way, from our view point. | 54 | Quiz Questions. 17. What assumption is | |
| Spiral Galaxy Dwingeloo 1. | made in determining mass by the rotation | ||
| 28 | Interacting Galaxies. Particularly in | curve method, the cluster method, and the | |
| rich clusters, galaxies can collide and | velocity dispersion method? a. That | ||
| interact. Galaxy collisions can produce | Newton's law of gravity is valid. b. That | ||
| ring galaxies and. tidal tails. Often | the system being measured is holding | ||
| triggering active star formation: | itself together. c. That spiral galaxies | ||
| starburst galaxies. Cartwheel Galaxy. NGC | rotate faster than elliptical galaxies. d. | ||
| 4038/4039. | Both a and b above. e. All of the above. | ||
| 29 | Tidal Tails. Computer simulations | 55 | Quiz Questions. 18. Which feature of a |
| produce similar structures. Example for | galaxy seems to be related to the mass of | ||
| galaxy interaction with tidal tails: The | the galaxy's central supermassive black | ||
| Mice. | hole? a. The size of the galaxy's central | ||
| 30 | Simulations of Galaxy Interactions. | bulge. b. The rotation curve of the | |
| Numerical simulations of galaxy | galaxy. c. The overall color of the | ||
| interactions have been very successful in | galaxy. d. The mass of the galaxy. e. The | ||
| reproducing tidal interactions like | age of the galaxy. | ||
| bridges, tidal tails, and rings. | 56 | Quiz Questions. 19. Which of the | |
| 31 | Mergers of Galaxies. Multiple nuclei | following is the least important factor in | |
| in giant elliptical galaxies. Radio image | galactic evolution? a. Collision of | ||
| of M 64: Central regions rotating | galaxies. b. The merger of larger | ||
| backward! NGC 7252: Probably result of | galaxies. c. The harassment by galaxies | ||
| merger of two galaxies, ~ a billion years | that pass nearby. d. Small galaxies are | ||
| ago: Small galaxy remnant in the center is | cannibalized by larger galaxies. e. The | ||
| rotating backward! | elemental composition of the material from | ||
| 32 | Galactic Cannibalism. Collisions of | which galaxies form. | |
| large with small galaxies often result in | 57 | Quiz Questions. 20. In a few billion | |
| complete disruption of the smaller galaxy. | years our own Milky Way may merge with the | ||
| Small galaxy is “swallowed” by the larger | Andromeda galaxy. Which type of galaxy is | ||
| one. This process is called “galactic | most likely to result from such a merger? | ||
| cannibalism”. NGC 5194. | a. An irregular galaxy. b. A larger spiral | ||
| 33 | Starburst Galaxies. Starburst galaxies | galaxy. c. An elliptical galaxy. d. Either | |
| are often very rich in gas and dust; | a or c above. e. Either b or c above. | ||
| bright in infrared: ultraluminous infrared | 58 | Answers. 1. c 2. e 3. a 4. c 5. e 6. e | |
| galaxies. M 82. Cocoon Galaxy. | 7. c 8. e 9. d 10. a. 11. e 12. a 13. a | ||
| 34 | Large Scale Structure. Superclusters = | 14. e 15. d 16. b 17. d 18. a 19. e 20. c. | |
| clusters of clusters of galaxies. | 59 | Hubble. (SLIDESHOW MODE ONLY). | |
| Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoints Slide Show mode (presentation mode).ppt | |||
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Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoints Slide Show mode (presentation mode)
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Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoints Slide Show mode (presentation mode)