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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