Today. Doppler Effect & Motion. Telescopes

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1 Today Doppler Effect & Motion Telescopes

2 The Doppler Effect Doppler ball 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

3 Doppler Effect for Light Motion away -> redshift Motion towards -> blueshift λ λ = λ obs λ em λ em = v c 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

4 Measuring the Shift Stationary Moving Away Away Faster Moving Toward Toward Faster We generally measure the Doppler effect from shifts in the wavelengths of spectral lines Pearson Education Inc., publishing as Pearson Addison-Wesley

5 Spectrum position along slit Doppler shift wavelength spectrograph slit

6 Doppler shift tells us ONLY about the part of an object s motion toward or away from us (along our line of sight). maximum doppler effect no doppler effect intermediate case 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

7 Telescopes Telescopes collect more light than our eyes light-collecting area Telescopes can see more detail than our eyes angular resolution (magnification) Telescopes/instruments can record light more sensitively than our eyes, and detect electromagnetic radiation that is invisible to our eyes (e.g., infrared, ultraviolet) 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

8 Bigger is better 1. Larger light-collecting area can see fainter things 2. Better angular resolution can see smaller things 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

9 Bigger is better For a telescope with mirror of diameter D, can see fainter: b 1 D 2 with higher resolution: θ λ D 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

10 Basic Telescope Design Refracting: lenses Refracting telescope Yerkes 1-m refractor 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

11 Basic Telescope Design Reflecting: mirrors Most research telescopes today are reflectors Reflecting telescope Gemini North 8-m 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

12 Kitt Peak National Observatory (AZ) 4 m

13 2.1 m WIYN (3.5 m) Burrell Schmidt

14

15 2.1 m

16 Inside 4 m dome

17 4 m

18 WIYN 3.5 m

19

20 Different designs for different wavelengths of light Radio telescope (Arecibo, Puerto Rico) Longer wavelengths need larger mirrors 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

21 Aricebo 305 m

22 Aricebo 305 m

23 Aricebo 305 m

24 GBT: 100 x 110 m receiver secondary Image courtesy of NRAO/AUI primary

25 Interferometry This technique allows two or more small telescopes to work together to obtain the angular resolution of a larger telescope. Very Large Array (VLA), New Mexico 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

26 Very Large Array (VLA), New Mexico angular resolution of a telescope this size 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

27 28 x 25 m EVLA 21 cm) CARMA 2.6 mm) 6.1 m 10.4 m 3.5 m

28 RADIO mm IR optical

29 X-ray telescope: grazing incidence optics 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

30 Advantages of telescopes in space Hubble Chandra 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

31 Observing problems due to Earth s atmosphere 1. Light Pollution 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

32 2. Atmospheric Turbulence causes twinkling blurs images (called seeing by astronomers). Star viewed with ground-based telescope View from Hubble Space Telescope 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

33 3. Atmosphere absorbs most of EM spectrum, including all UV and X ray and most infrared. Fermi Herschel 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

34 Telescopes in space solve all 3 problems. Chandra X-ray Observatory 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

35 Instruments Cameras Pearson Education Inc., publishing as Pearson Addison-Wesley

36 Dark Energy Camera 570 Megapixel

37 CCD imager + friends LN2 dewar

38 NGC bright spiral Hα emission line (pink) traces recent Star Formation

39 SQIID (older IR imager) at 4m Cassegrain focus 3 x 3 FOV

40 SQIID

41 NEWFIRM near-ir imager 28 x 28 FOV

42 Kitt Peak 4m + NEWFIRM K -band (2.2 micron) Stellar mass maps from near-ir data (2.2 or 3.6 microns) F561-1 F563-V1 D564-9 D570-7

43 Instruments grating Spectrographs 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley

44

45 slit view

46 spectrograph

47 grating

48 spectrograph slit NGC 2683

49 Spectrum position along slit Doppler shift wavelength

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