1 / 43

LECTURE 22, NOVEMBER 18, 2010

LECTURE 22, NOVEMBER 18, 2010. ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT jcbrandt@unm.edu. Question 2. a) ongoing star formation b) a disk, bulge, and halo c) globular clusters in the halo d) open clusters in the disk e) all of the above. What property is shared by spiral galaxies?.

gilead
Download Presentation

LECTURE 22, NOVEMBER 18, 2010

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. LECTURE 22, NOVEMBER 18, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT jcbrandt@unm.edu ASTR 101-3, FALL 2010

  2. ASTR 101-3, FALL 2010

  3. ASTR 101-3, FALL 2010

  4. ASTR 101-3, FALL 2010

  5. ASTR 101-3, FALL 2010

  6. ASTR 101-3, FALL 2010

  7. ASTR 101-3, FALL 2010

  8. ASTR 101-3, FALL 2010

  9. ASTR 101-3, FALL 2010

  10. ASTR 101-3, FALL 2010

  11. Question 2 a) ongoing star formation b) a disk, bulge, and halo c) globular clusters in the halo d) open clusters in the disk e) all of the above What property is shared by spiral galaxies? ASTR 101-3, FALL 2010

  12. Question 2 a) ongoing star formation b) a disk, bulge, and halo c) globular clusters in the halo d) open clusters in the disk e) all of the above What property is shared by spiral galaxies? M-51, a Type Sb spiral ASTR 101-3, FALL 2010

  13. Question 3 a) giant globular clusters in the halo. b) small irregular galaxies that orbit the Milky Way. c) large molecular clouds in the disk of our Galaxy. d) the brightest ionized hydrogen regions in our Galaxy. e) spiral nebulae originally discovered by Herschel. The Magellanic Clouds are ASTR 101-3, FALL 2010

  14. Question 3 a) giant globular clusters in the halo. b) small irregular galaxies that orbit the Milky Way. c) large molecular clouds in the disk of our Galaxy. d) the brightest ionized hydrogen regions in our Galaxy. e) spiral nebulae originally discovered by Herschel. The Magellanic Clouds are ASTR 101-3, FALL 2010

  15. ASTR 101-3, FALL 2010

  16. ASTR 101-3, FALL 2010

  17. ASTR 101-3, FALL 2010

  18. ASTR 101-3, FALL 2010

  19. ASTR 101-3, FALL 2010

  20. ASTR 101-3, FALL 2010

  21. ASTR 101-3, FALL 2010

  22. ASTR 101-3, FALL 2010

  23. Question 5 a) more distant galaxies showing greater blueshifts. b) distant quasars appearing proportionally dimmer. c) more distant galaxies showing greater redshifts. d) slowly varying Cepheid variables appearing brighter. e) more distant galaxies appearing younger. Hubble’s law is based on ASTR 101-3, FALL 2010

  24. Question 5 a) more distant galaxies showing greater blueshifts. b) distant quasars appearing proportionally dimmer. c) more distant galaxies showing greater redshifts. d) slowly varying Cepheid variables appearing brighter. e) more distant galaxies appearing younger. Hubble’s law is based on ASTR 101-3, FALL 2010

  25. Question 6 a) the density of galaxies in the universe. b) the luminosity of distant galaxies. c) the reddening of light from dust clouds. d) the speed of a galaxy. e) the rate of expansion of the universe. Hubble’s constant measures ASTR 101-3, FALL 2010

  26. Question 6 a) the density of galaxies in the universe. b) the luminosity of distant galaxies. c) the reddening of light from dust clouds. d) the speed of a galaxy. e) the rate of expansion of the universe. Hubble’s constant measures Hubble’s law relates how fast galaxies are moving away from us at different distances. A larger value for H0 implies a faster expansion rate. Velocity = H0 x Distance ASTR 101-3, FALL 2010

  27. Question 7 a) the size of the universe. b) distances to galaxies. c) the speed of recession of galaxies. d) the density of matter in the universe. e) the temperature of the Big Bang. To calibrate Hubble’s constant, astronomers must determine ASTR 101-3, FALL 2010

  28. Question 7 a) the size of the universe. b) distances to galaxies. c) the speed of recession of galaxies. d) the density of matter in the universe. e) the temperature of the Big Bang. To calibrate Hubble’s constant, astronomers must determine Distances to galaxies are determined using a variety of “standard candles,” including Cepheid variables, supernova explosions, model galaxies, and model clusters. ASTR 101-3, FALL 2010

  29. ASTR 101-3, FALL 2010

  30. ASTR 101-3, FALL 2010

  31. ASTR 101-3, FALL 2010

  32. ASTR 101-3, FALL 2010

  33. ASTR 101-3, FALL 2010

  34. ASTR 101-3, FALL 2010

  35. ASTR 101-3, FALL 2010

  36. ASTR 101-3, FALL 2010

  37. ASTR 101-3, FALL 2010

  38. ASTR 101-3, FALL 2010

  39. ASTR 101-3, FALL 2010

  40. Question 10 a) supermassive black holes at their cores. b) dark matter. c) self-sustaining star formation. d) spiral density waves. e) hypernova explosions. Seyfert and radio galaxies could be powered by ASTR 101-3, FALL 2010

  41. Question 10 a) supermassive black holes at their cores. b) dark matter. c) self-sustaining star formation. d) spiral density waves. e) hypernova explosions. Seyfert and radio galaxies could be powered by The Circinus Galaxy, a Seyfert galaxy about 4 Mpc away ASTR 101-3, FALL 2010

  42. ASTR 101-3, FALL 2010

  43. ASTR 101-3, FALL 2010

More Related