Lecture Fall, 2005 Astronomy 110 1

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1 Lecture Fall, 2005 Astronomy 110 1

2 Important Concepts for Understanding Spectra Electromagnetic Spectrum Continuous Spectrum Absorption Spectrum Emission Spectrum Emission line Wavelength, Frequency Fall, 2005 Astronomy 110 2

3 What can we learn from light? Temperature: What is Black Body Radiation A Black body emits equally well at all wavelengths. An idealization to help model the interaction of light with matter. Black body or Thermal Radiation Objects that interact with electromagnetic energy emit thermal radiation. This includes stars, planets, you An object s thermal radiation spectrum depends on only one property: its temperature Fall, 2005 Astronomy 110 3

4 Two Properties of Thermal Radiation: As the temperature increases: more BB energy per unit area is radiated at all frequencies. photons with a higher average energy (higher f) are emitted. the peak of the BB spectrum shifts towards shorter wavelengths. Fall, 2005 Astronomy 110 4

5 Spectra A real object has a spectrum that is a mix of thermal (black body) and discrete (line) features. Fall, 2005 Astronomy 110 5

6 Thought Question Which is hotter? a) A blue star. b) A red star. c) A planet that emits only infrared light. Fall, 2005 Astronomy 110 6

7 Which is hotter? a) A blue star. b) A red star. c) A planet that emits only infrared light. Fall, 2005 Astronomy 110 7

8 Thought Question Why don t we glow in the dark? a) People do not emit any kind of light. b) People only emit light that is invisible to our eyes. c) People are too small to emit enough light for us to see. d) People do not contain enough radioactive material. Fall, 2005 Astronomy 110 8

9 Why don t we glow in the dark? a) People do not emit any kind of light. b) People only emit light that is invisible to our eyes. c) People are too small to emit enough light for us to see. d) People do not contain enough radioactive material. Fall, 2005 Astronomy 110 9

10 What can we learn from light? Speed: What is the Doppler Effect? The Doppler Effect. Fall, 2005 Astronomy

11 The Doppler Effect Motion toward or away from an observer causes a shift in the observed wavelength of light: blueshift (shorter wavelength) motion toward you redshift (longer wavelength) motion toward you greater shift greater speed Fall, 2005 Astronomy

12 The Doppler Effect Fall, 2005 Astronomy

13 Same for Light Fall, 2005 Astronomy

14 The amount of blue or red shift tells us an object s speed toward or away from us: Fall, 2005 Astronomy

15 Doppler shift tells us ONLY about the part of an object s motion toward or away from us: Fall, 2005 Astronomy

16 Thought Question: A spectral line is measured in the lab at nm. The same line in a star has wavelength of 502.8nm. What can we say about this star? a) It is moving away from me. b) It is moving towards me. c) It has unusually long spectral lines. Fall, 2005 Astronomy

17 I measure a line in the lab at nm. The same line in a star has wavelength nm. What can I say about this star? a) It is moving away from me. b) It is moving towards me. c) It has unusually long spectral lines. Fall, 2005 Astronomy

18 Measuring Redshift Fall, 2005 Astronomy

19 Measuring Velocity Fall, 2005 Astronomy

20 Learning from Light: Types of Spectra Thermal radiation spectrum continuous Absorption line spectrum specific frequencies are missing. Emission line spectrum light only at specific energies. Fall, 2005 Astronomy

21 Learning from Light: Composition Temperature We determine composition from spectral lines. We can determine temperature from the spectrum of thermal radiation Fall, 2005 Astronomy

22 Learning from Light: Speed The Doppler effect tells us how fast an object is moving toward or away from us. Blueshift:objects moving toward us Redshift: objects moving away from us Fall, 2005 Astronomy

23 Telescopes Fall, 2005 Astronomy

24 Why do we need Telescopes? Telescopes collect more light than our eyes Sensitivity Telescopes can see more detail than our eyes angular resolution Telescopes/instruments can detect light that is invisible to our eyes (e.g., infrared, ultraviolet) Fall, 2005 Astronomy

25 Bigger is better Fall, 2005 Astronomy

26 Angular Resolution The minimum angular separation that the telescope can distinguish. Fall, 2005 Astronomy

27 Angular resolution: smaller is better Fall, 2005 Astronomy

28 Fall, 2005 Astronomy

29 Basic Telescope Design Refracting: lenses Refracting telescope Yerkes 1-m refractor Fall, 2005 Astronomy

30 Basic Telescope Design Reflecting: mirrors Most research telescopes. Reflecting telescope Gemini North 8-m Fall, 2005 Astronomy

31 Keck I and Keck II - Mauna Kea, HI Fall, 2005 Astronomy

32 Fall, 2005 Astronomy

33 Mauna Kea, Hawaii Fall, 2005 Astronomy

34 Different designs for different wavelengths of light Radio telescope (Arecibo, Puerto Rico) Fall, 2005 Astronomy

35 X-ray telescope: grazing incidence optics Fall, 2005 Astronomy

36 Telescopes in Space Fall, 2005 Astronomy

37 Radio IR VIS X-Ray Fall, 2005 Astronomy

38 Observing problems due to Earth s atmosphere 1. Light Pollution Fall, 2005 Astronomy

39 2. Turbulence causes twinkling blurs images. Star viewed with ground-based telescope View from Hubble Space Telescope Fall, 2005 Astronomy

40 3. Atmosphere absorbs most of EM spectrum, including all UV and X-ray, most infrared Fall, 2005 Astronomy

41 How is technology revolutionizing astronomy? adaptive optics Rapid changes in mirror shape compensate for atmospheric turbulence. Without adaptive optics With adaptive optics Fall, 2005 Astronomy

42 Adaptive Optics at Gemini South Hokupa`a Fall, 2005 Astronomy

43 Fall, 2005 Astronomy

44 interferometry Allows two or more small telescopes to work together to obtain the angular resolution of a larger telescope. Very Large Array (VLA), New Mexico Fall, 2005 Astronomy

45 Fall, 2005 Astronomy

46 The Moon might be a great spot for an observatory - but at what price? Fall, 2005 Astronomy

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