1. Astronomy 1010-H Planetary Astronomy Fall_2015 Day-23

3. Course Announcements How is the sunset/sunrise observing going? SW-chapter 6 posted: due Fri. Oct. 23 1 st Quarter Observing night: Tuesday, Oct. 20; 7:30pm

4.  Electronic detectors record photons on pixels.  Photons create a signal in the array.  CCDs = charge-coupled devices (such as digital cameras).

5.  The electronically recorded images can greatly exceed photographs in quality.  CCD = astronomer’s detector of choice.

6. Red Green Blue

7. Red Green Blue

8. Color separation is useful in a prism so that we can obtain a spectrum of light Since it is meant to be separated we don’t call it an aberration. Instead, it is called dispersion

9.  Spectrographs disperse the incoming light into its component wavelengths.  Lets astronomers study the spectrum of an object’s light.

10. A diffraction grating works on interference of light waves Diffraction is much more efficient at separating light into its colors than dispersion

11. Unfortunately, diffraction also leads to problems Look closely enough at stars and they aren’t just points of light but rings, too

12. The best spectrographs use diffraction gratings

13. The spectrograph/CCD produces a black & white spectrum

14. Multitasking Saves Time

15. Spectrum But visible light is only one type of electromagnetic radiation (light) emitted by stars Astronomers are truly interested in the entire spectrum of Light!

16.  The atmosphere does not transmit all light.  Nearly all X-ray, ultraviolet, and infrared wavelengths are blocked.  Satellites are needed for these wavelengths.

17. Consider This Class as Seen in Different Wavelengths of Light!

18. Orion in Infrared!

19. HST Views of Orion Nebula showing stars hidden in clouds http://oposite.stsci.edu/pubinfo/pr/97/13/A.html

20. Observations at other wavelengths are revealing previously invisible sights UV Ordinary visible Infrared Map of Orion region

21.  Radio telescopes are large, steerable parabolic dishes with antennas.  Allow astronomers to study radio waves.  Wavelengths of a centimeter to about 10 meters.  Radio waves can pass through gas and dust.

22. Radio wavelength observations are possible from Earth’s surface

23. Observing with Radio Waves Long Wavelength…poor resolution

24. Under the dish at Arecibo

25. The Very Large Array (VLA)

26.  Single radio telescopes have poor resolution due to the long wavelengths.  Interferometric arrays combine the signals from many telescopes, increasing resolution.

27.  Two electromagnetic waves in the same location will produce interference.  The waves will either enhance or detract from each other, resulting in constructive or destructive interference.  This can result in spectral dispersion. CONNECTIONS 6.2