1. Orbits and Galaxy Shape elliptical orbits random orientations different speeds in different directions

2. Orbits and Galaxy Shape Halo and Bulge: elliptical orbits random orientations Disk: nearly circular orbits same direction a little “bobbing” up and down

3. Thought Question: Which of the following mergers of spiral and elliptical galaxies is most unlikely?

4. orderly orbits in spiral galaxies are disrupted during collisions:

5. collisions between galaxies affect star orbits many examples – especially in galaxy clusters Environment

7. Stars versus Gas “Collisions” of star groups don’t result in star collisions… stars are small with lots of space between BEFOREAFTER Collisions of gas clouds result in “shocks” … kinetic energy converted to heat and radiated away

8. Galaxy Properties SpiralElliptical Shapesflat disk + round bulge elliptical (football) Overall colorbluish (young, high-mass stars) reddish (giant stars) Gas, Dustyes – in disklittle or none Where?mostly in emptier regions of space often in clusters of galaxies

9. Zoom in on a seemingly blank piece of sky…

10. Observe galaxies to try to learn… what does the universe look like? what was its past? what is its future? Cosmology

11. How Does the Universe Look? Isotropic?: Does it look almost the same in all directions to us?  count galaxies in different directions Homogeneous?: Would it look almost the same to observers anywhere?  measure distances to many galaxies

12. How Does the Universe Look? I feel left out… Isotropic?: Does it look almost the same in all directions to us?  count galaxies in different directions Homogeneous?: Would it look almost the same to observers anywhere?  measure distances to many galaxies

13. Thought Question Which of these 4 universes is homogeneous? (Enter the letters for all correct answers.)

14. Thought Question Which of these 4 universes is isotropic according to the stick figure? (Enter the letters for all correct answers.)

15. Is the Universe Isotropic? isotropic: looks the same in all directions to us All-sky surveys of millions of galaxies show there are no special directions blocking by Milky Way

16. Is the Universe Homogeneous?  harder to measure: need to measure galaxy distances and survey faint, distant galaxies some “clumping” of galaxies on small scales, but there seem to be no special places

17. Is the Universe Homogeneous? galaxies line up in filaments, with clumps where they meet

21. EVIDENCE: Expansion of the Universe (1928) Almost all galaxies have redshifts  appear to be moving away from us  more distant galaxies have larger redshifts… BLUERED BLUE

22. COINCIDENCE? HMMM… WHEW! DID SOMETHING DIE IN HERE?

23. Hubble’s Law v r : recession velocity d: distance H 0 : Hubble constant 22 km/s / Mly (1 Mly = 1 Mega light-year = 10 6 light-years)

24. Hubble’s Law (fast forward)

25. Consequence #1 what we see: alien galaxy feels stationary to them they observe the same Hubble Law!

26. Consequence #2 All distances change by the same percentage in the same time:  implies space is stretching uniformly to make Hubble’s Law

27. Imagine running time backwards:  galaxies would meet in same place at same time t in past (BIG BANG) Consequence #3

28. THEORY: A “Big Bang” Idea: universe had a beginning early universe was hot, dense gas Tests: Did “Big Bang” leave evidence? THEORY: a scientific idea that has survived repeated tests of its predictions

29. Evidence for a “Big Bang” What clues do we have that there was a BEGINNING to the Universe? Dark Sky at Night Expansion of the Universe (Hubble’s Law) Cosmic Microwave Background Radiation Abundances of Chemical Elements

30. The Observable Universe If universe is NOT infinitely old, then…  only see galaxies whose light had time to reach us  universe may be MUCH larger, but there’s an edge (“HORIZON”) to what we can see  more distant galaxies look younger to us: “LOOKBACK TIME” OBSERVABLE UNIVERSE UNOBSERVABLE UNIVERSE

31. Thought Question: Imagine you are observing a high-mass star located in a distant galaxy 100 million light-years away. By analyzing the starlight, you are able to tell that the star appears to be 10 million years old. From its properties, you predict that the star has a total lifetime of 50 million years. How long before we receive light from this star’s supernova? 100 MILLION LIGHT-YEARS ? “I see a blue star right now.” (Enter your answers in millions of yrs.)

32. Thought Question: Imagine you are observing a high-mass star located in a distant galaxy 100 million light-years away. By analyzing the starlight, you are able to tell that the star appears to be 10 million years old. From its properties, you predict that the star has a total lifetime of 50 million years. When will or when did the supernova actually occur? 100 MILLION LIGHT-YEARS ? “I see a blue star right now.” (Enter your answers in millions of yrs. If it already happened, make your answer negative.)

33. Lookback 100 MILLION LIGHT-YEARS 40 MILLION LIGHT-YEARS “The star just blew up!!!” “The star has been dead for 60 million years.” “The star looks like it has 40 million years to live.”

34. “DARK AGES” UNOBSERVABLE UNIVERSE (early in history) How far back in time can we possibly look? “DARK AGES”: before galaxies and stars were born Universe was once OPAQUE  gas too dense to let light through Universe History US

35. Stretching and Redshifts Redshift tells us about total amount of stretching universe has done while the light has been traveling EXPANDING UNIVERSE: PRESENT DISTANT PAST MEDIUM PAST  LARGER REDSHIFT FOR MORE DISTANT GALAXY

36. Universe Scale We can’t measure size of universe (especially if infinite), so compare distances at different times in history: Distances between non-moving galaxies stretch in same way light wavelengths do: PRESENT: PAST: density of the universe was larger in the past: R U =1 z=0: present R U 1: past

37. Thought Question: The most distant object that has been seen has a redshift of about z = 8. Roughly how far was it from us when it released the light we see today? A.9 times its present distance B.8 times its present distance C.7 times its present distance D.Its present distance E.1/7th its present distance F.1/8th its present distance G.1/9th its present distance

38. EVIDENCE: Cosmic Microwave Background Radiation (1965)  Microwave and radio from all directions in sky with nearly equal brightness: MAP OF ENTIRE SKY:  thermal radiation with very low temperature T = 2.728 K

39. EVIDENCE: Cosmic Microwave Background Radiation (1965)  If Big Bang was an explosion at one place in space, we should see a glow only from that place…  BIG BANG seems to have happened EVERYWHERE

40. Cosmic Microwave Background Radiation  thermal radiation with temperature T = 2.728 K Expansion of universe stretches light, made temperature lower today:

41. The Horizon Problem Opposite sides of observable universe somehow “knew” to have almost the same temperature today  takes longer than age of universe for light to travel from one side to the other… HORIZON Choose a number between 1 and 1 million. 538,68 1

42. INFLATION: age 10 -35 s to 10 -32 s  space expands faster than light can travel by huge amount (10 50 times)  parts of then-observable universe move so far away we never see them again  needed to explain:  isotropic microwave background  homogeneous universe History of the Universe OUR OBSERVABLE UNIVERSE TODAY THEN-OBSERVABLE UNIVERSE (BEFORE INFLATION) OBSERVABLE UNIVERSE AFTER INFLATION BEFORE: AFTER: