1. Chapter 4: Telescopes

3. E O Optical telescopes: Reflectors and refractors Refractors use lenses E: eyepiece O: objective

4. Reflectors use mirrors: Newtonian Cassegrain

5. Objective (O) = Main light-gathering surface (lens or mirror) Aperture = a = Diameter of objective ("size" of telescope) Focal length = f = Distance from objective to image ("length" of telescope) Eyepiece (E) = Lens used to inspect image from objective

6. 1) LIGHT GATHERING POWER (how faint you can see) LGP ~ a 2 (Bigger = better) 2) MAGNIFYING POWER (how large image is) MP = f(O) / f(E)(Bigger = better) So can change this with eyepice choice, not a fundamental property of telescope Practical limit  50 x O (in inches) 3) RESOLVING POWER (size of detail, sharpness of focus) Size of detail ~ 1/a(Smaller = better) i.e., larger ‘a’ allows smaller details to be seen

8. Resolution vs. magnification

10. Airy disk. Light coming through a circular aperture

13. Resolution vs. magnification

14. Atmospheric seeing

16. The planet Uranus imaged in the infrared

17. Spitzer Space Telescope An infrared telescope in orbit around the Sun!

19. 43 m diameter

22. How to improve resolution? Radio interferometry The Very Large Array, Socorro, New Mexico

23. VLBI

24. Chandra Xray observatory

25. X-ray telescope design (Chandra X-ray Observatory) It is very difficult to focus (redirect) high energy photons, because they are so readily absorbed by matter. Thus it is difficult to tell where they came from, and to reconstruct the image.

26. Chandra image of X-rays emitted from hot gas surrounding galaxy Cygnus-A

27. An Xray image of a black hole, by Chandra.

28. X-ray image Visible (optical) Hot stars give off a lot more Xrays than cooler stars do.

29. Observing gamma rays Space-based telescopes (Compton Gamma ray Observatory