1. Studying for the Exam Relevant chapters: E, 1, 2 & 3 To prepare for the exam it is helpful to … –review readings –review lecture notes online (esp. concept questions) –revisit homework –look over the activities

2. Studying for the Exam Filter out the relevant information, don’t focus on details Properties of relevant information: –Information appears repeatedly in course materials (readings, slides, homework,…) –It is not an isolated fact, but can be “reasoned out” –It is an important concept (e.g. daily & monthly motion, scientific method)

3. Exam Questions About 30 multiple choice questions A few short answer problems Types of questions NOT on the exam: –What’s Galileo’s birth year? –What is the frequency of yellow light? –What is the distance of the Earth to the Sun? –What is the mathematical formula for the Hydrogen energy levels?

4. Exam Questions Types of questions that could be on the exam: –Why isn’t there a lunar eclipse every full moon? –It is noon in Westerville. Is it earlier/ later/different day/different season in Paris, France? –What is the difference between a sidereal and a solar day? –How high above the horizon is the polar star at noon if you are at 23 degrees northern latitude? –Given the wavelength of yellow light, what is its frequency?

5. Doppler Shift From Wikipedia

6. Doppler Shift Can use the Doppler shift to determine radial velocity of distant objects relative to us Transverse velocity can be measured from the motion of stars with respect to back- ground over a period of years

7. Homework: Doppler Shift of Hydrogen spectrum The discrepancy between the wavelength of a line measured in the lab versus measured on an object is proportional to the velocity of the object Apparent/ true wavelength = 1+ velocity/c Example: –Observed(or apparent): 698 nm –Actual(or true or lab) wavelength: 656.3nm –velocity = (698nm/656.3nm -1) c = 19100 km/s

8. Atomic Energy Levels For Hydrogen, the energies of the atomic levels are given by a simple formula that just depends on the (excitation) number n of the orbit: E n = – Ry / n 2 where Ry = 13.6 eV = 2.179 x 10 -18 J  E 1, E 2 =¼ E 1, E 3 =1/9 E 1,… Electrons in higher levels will cascade down, producing many different spectral lines Formula can be converted to frequency, wavelength

9. Light hits Matter: Refraction Light travels at different speeds in vacuum, air, and other substances When light hits the material at an angle, part of it slows down while the rest continues at the original speed – results in a change of direction –Different colors bend different amounts – prism, rainbow

10. Application for Refraction Lenses use refraction to focus light to a single spot

11. Light hits Matter (II): Reflection Light that hits a mirror is reflected at the same angle it was incident from Proper design of a mirror (the shape of a parabola) can focus all rays incident on the mirror to a single place

12. Application for Reflection Curved mirrors use reflection to focus light to a single spot

13. Telescopes From Galileo to Hubble

14. Telescopes Light collectors Two types: –Reflectors (Mirrors) –Refractors (Lenses) Magnification: –ratio of focal lengths of objective and eyepiece –M = f obj /f eye –Example: 2000mm telescope with 40mm eyepiece: 50x

15. Reflecting Telescopes

16. Problems with Refractors Different colors (wavelengths) bent by different amounts – chromatic aberration Other forms of aberration Deform under their own weight Absorption of light Have two surfaces that must be optically perfect

17. Telescope Size A larger telescope gathers more light (more collecting area) Angular resolution is limited by diffraction of light waves; this also improves with larger telescope size

18. Resolving Power of Telescopes Andromeda Galaxy Telescope 1 Telescope 2 of double size

19. Resolving Power of Telescopes (II) Andromeda Galaxy Resolution: (a)10’ (b)1’ (c)5” (d)1”

20. Magnification The magnification of a telescope can easily be changed by plugging in a different eyepiece with a different focal length M= focal length of main lens or mirror focal length of eyepiece Example: F= 2000mm, f = 40 mm  M= 50

21. Atmospheric Limitations

22. Radio Window Optical Window IR Window

23. Largest Earth-Based Telescopes Hobby-Eberly Telescope, Davis Mountains, TX –11 m diameter –Cannot see all parts of the sky Keck I and II, Mauna Kea, HI –36  1.8 m hexagonal mirrors; equivalent to 10 m –Above most of atmosphere (almost 14,000 ft ASL) –Operating since 1993

24. Other Techniques Put telescopes on satellites –Hubble Space Telescope: 2.4 m, since 1990 Use computers to correct optics during light gathering: adaptive and active optics Interferometry Radio astronomy

25. Other Wavelengths Must be carried out on satellites (or rockets, balloons, etc.) due to strong absorption in the atmosphere Infrared astronomy High-energy (UV, X-ray, gamma-ray) astronomy

26. Full-Spectrum Coverage  Each region of the electromagnetic spectrum gives us valuable information about the universe (only these frequency bands can be observed with ground- based telescopes) Radio Infrared Visible X-Ray Gamma -ray