1. Chapter 5 Telescopes: “light bucket”

2. Telescopes have three functions 1.Gather as much light as possible: LGP ∝ Area = πR 2 LGP ∝ Area = πR 2 Why? Why? UVIR Energy Output Wavelength

3. The light gathering power is proportional to the area

4. Telescopes have three functions 2. Resolve objects: Θ = 0.25 ( λ/D) Why? In astronomy, we are always concerned with angular measurement “close together” means “separated by a small angle on the sky,” angular resolution is the factor that determines our ability to see fine structure

5. Telescopes have three functions 3. Magnify EXTENDED objects. Why? Extended objects: The most surprising property is that extended objects do not get brighter in a scope. Also the contrast does not change (actually it only can get worse). The only thing that changes is that the object itself gets bigger by magnification

6. Reflection is the bouncing of light off a surface

7. How do we see an object Light rays coming from one point of an object are focused at one point at the back of your eye Light rays coming from one point of an object are focused at one point at the back of your eye (retina). (retina). Different points from an object are focused at different points of your retina. Different points from an object are focused at different points of your retina.  So we see an image of the object produced by the lense in our eyes at the back of our eye.

8. A telescope is not a microscope Microscope’s function is magnification Telescope’s function is gathering as much light as possible: Large lenses Large lenses do not result in larger magnification

9. The refracting telescope uses two lenses. Where is the image of the star? Light Bending

10. Problem with refraction Different color light is refracted at different angles, causing a distortion of the image Different color light is refracted at different angles, causing a distortion of the image

11. Refractors suffer from Chromatic Aberration

12. Dispersive refraction leads to chromatic aberration: More on chromatic aberration CLL: Diffraction Rings

13. Chromatic Aberration

14. Images can be formed through reflection or refraction Reflecting mirror

15. Image formation Where do you stand to observe the object? What’s the problem with that? How to overcome the problem?

16. Types of reflecting telescopes: To get around the blocking of light when you stand in the focal plane, different telescope types were invented

17. Do reflecting optical devices suffer from chromatic aberration A)Yes, different color light reflects at different angles and therefore focuses at different points. B)No, different color light reflects always at the same angle as it incidents, causing no chromatic aberration.

18. But: Spherical mirrors suffer from Spherical Aberration Parallel light from different locations of the mirror is not exactly focused at one point

19. Spherical aberration can be eliminated by a parabolic shape or a corrector plate CLL: Focus of a Cassegrain reflectorFocus of a Cassegrain reflector

21. Optical Telescopes The Keck telescope, a modern research telescope:

22. Optical Telescopes The Hubble Space Telescope has a variety of detectors:

23. Discovery 5-1: The Hubble Space Telescope The Hubble Space Telescope’s main mirror is 2.4 m in diameter and is designed for visible, infrared, and ultraviolet radiation

24. Discovery 5-1: The Hubble Space Telescope Here we compare the best ground-based image of M100, on the left, with the Hubble image on the right

25. In astronomy, we are always concerned with angular measurement “close together” means “separated by a small angle on the sky,” angular resolution is the factor that determines our ability to see fine structure Protractor-string Example

26. Light-gathering power: Improves detail Brightness proportional to square of radius of mirror Below: (b) was taken with a telescope twice the size of (a) Telescope Size

27. Resolving power: When better, can distinguish objects that are closer together Resolution is proportional to wavelength and inversely proportional to telescope size—bigger is better! Telescope Size

28. Resolution Want to resolve objects which are close together. Want to resolve objects which are close together. Objects that are close together are separated by a smaller angle than objects that are at the same distance but further apart. Objects that are close together are separated by a smaller angle than objects that are at the same distance but further apart. Θ = 2.06 X 10 5 ( λ/D) Θ = 2.06 X 10 5 ( λ/D) Smaller the better

29. How to improve the resolution? A) Increase the size of the mirror B) Decrease the size of the mirror C) Use light with smaller wavelength D) Use light with larger wavelength Smaller the better For comparison, the angular resolution of the human eye in the middle of the visual range is about 0.5'.

30. What limits a telescope’s resolution? One important factor is diffraction, the tendency of light, and all other waves to bend around corners Diffraction introduces a certain “fuzziness,” or loss of resolution

31. Effect of improving resolution: (a) 10′; (b) 1′; (c) 5″; (d) 1″ 5.2 Telescope Size

32. Image acquisition: Charge-coupled devices (CCDs) are electronic devices, can be quickly read out and reset 5.3 Images and Detectors

33. Photometry is a technique of astronomy concerned with measuring the flux, or intensity of an astronomical object's electromagnetic radiation

34. Image processing by computers can sharpen images 5.3 Images and Detectors

35. Atmospheric blurring: Due to air movements 5.4 High-Resolution Astronomy

36. “Seeing”

37. Solutions: Put telescopes on mountaintops, especially in deserts Put telescopes in space 5.4 High-Resolution Astronomy

38. Active optics: Control mirrors based on temperature and orientation 5.4 High-Resolution Astronomy

39. Adaptive optics: Track atmospheric changes with laser; adjust mirrors in real time 5.4 High-Resolution Astronomy

40. These images show the improvements possible with adaptive optics:

41. Radio telescopes: Similar to optical reflecting telescopes Prime focus Less sensitive to imperfections (due to longer wavelength); can be made very large 5.5 Radio Astronomy

42. Largest radio telescope: 300-m dish at Arecibo 5.5 Radio Astronomy

43. Longer wavelength means poor angular resolution Advantages of radio astronomy: Can observe 24 hours a day Clouds, rain, and snow don’t interfere Observations at an entirely different frequency; get totally different information 5.5 Radio Astronomy

44. Interferometry: Combine information from several widely spread radio telescopes as if they came from a single dish Resolution will be that of dish whose diameter = largest separation between dishes 5.6 Interferometry

45. Interferometry involves combining signals from two receivers; the amount of interference depends on the direction of the signal

46. Can get radio images whose resolution is close to optical Interferometry can also be done with visible light but is much more difficult due to shorter wavelengths 5.6 Interferometry

47. Infrared radiation can image where visible radiation is blocked; generally can use optical telescope mirrors and lenses 5.7 Space-Based Astronomy

48. Infrared telescopes can also be in space; the image on the left is from the Infrared Astronomy Satellite 5.7 Space-Based Astronomy

49. The Spitzer Space Telescope, an infrared telescope, is in orbit around the Sun. These are some of its images. 5.7 Space-Based Astronomy

50. Ultraviolet observing must be done in space, as the atmosphere absorbs almost all ultraviolet rays. 5.7 Space-Based Astronomy

51. X-rays and gamma rays will not reflect off mirrors as other wavelengths do; need new techniques X-rays will reflect at a very shallow angle and can therefore be focused 5.7 Space-Based Astronomy

52. X-ray image of supernova remnant 5.7 Space-Based Astronomy

53. Gamma rays cannot be focused at all; images are therefore coarse 5.7 Space-Based Astronomy

54. Much can be learned from observing the same astronomical object at many wavelengths. Here, the Milky Way: 5.8 Full-Spectrum Coverage

55. Refracting telescopes make images with a lens Reflecting telescopes with a mirror Modern research telescopes are all reflectors CCDs are used for data collection Data can be formed into image, analyzed spectroscopically, or used to measure intensity Large telescopes gather much more light, allowing study of very faint sources Large telescopes also have better resolution Summary of Chapter 5

56. Resolution of ground-based optical telescopes is limited by atmospheric effects Resolution of radio or space-based telescopes is limited by diffraction Active and adaptive optics can minimize atmospheric effects Radio telescopes need large collection area; diffraction limited Interferometry can greatly improve resolution Summary of Chapter 5 (cont.)

57. Infrared and ultraviolet telescopes are similar to optical Ultraviolet telescopes must be above atmosphere X-rays can be focused, but very differently than visible light Gamma rays can be detected but not imaged Summary of Chapter 5 (cont.)