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Astronomy: A Beginner’sGuide to the Universe
Seventh Edition
© 2013 Pearson Education, Inc.
Chapter 3 Lecture
Telescopes
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Chapter 3 Telescopes
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Units of Chapter 3
Optical Telescopes
Telescope Size
High-Resolution Astronomy
Radio Astronomy
Other Astronomies
Summary of Chapter 3
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Images can be formed through reflection or refraction.
Reflecting mirror
3.1 Optical Telescopes
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Refracting lens
3.1 Optical Telescopes
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3.1 Optical Telescopes
Image formation
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Reflecting and refracting telescopes
3.1 Optical Telescopes
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Modern telescopes are all reflectors:
• Light traveling through lens is refracted differently depending on wavelength.
• Some light traveling through lens is absorbed.
• Large lens can be very heavy, and can only be supported at edge.
• Lens needs two optically acceptable surfaces, mirror only needs one.
3.1 Optical Telescopes
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Types of reflecting telescopes
3.1 Optical Telescopes
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3.1 Optical Telescopes
Details of the Keck telescope
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Image acquisition: Charge-coupled devices (CCDs) are electronic devices, can be quickly read out and reset.
3.1 Optical Telescopes
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Image processing by computers can sharpen images.
3.1 Optical Telescopes
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The Hubble Space Telescope has several instruments.
Discovery 3-1: The Hubble Space Telescope
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Resolution achievable by the Hubble Space Telescope
Discovery 3-1: The Hubble Space Telescope
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Light-gathering power:
Improves detail
Brightness proportional to square of radius of mirror
The figure, part (b) was taken with a telescope twice the size of (a)
3.2 Telescope Size
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Multiple telescopes: Mauna Kea
3.2 Telescope Size
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3.2 Telescope Size
The VLT (Very Large Telescope), Atacama, Chile
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Resolving power: When better, can distinguish objects that are closer together.
Resolution is proportional to wavelength and inversely proportional to telescope size.
3.2 Telescope Size
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Effect of improving resolution:(a) 10; (b) 1; (c) 5; (d) 1
3.2 Telescope Size
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Atmospheric blurring due to air movements
3.3 High-Resolution Astronomy
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Solutions:• Put telescopes on mountaintops, especially in deserts.• Put telescopes in space.• Active optics – control mirrors based on temperature and orientation.
3.3 High-Resolution Astronomy
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Radio telescopes:• Similar to optical reflecting telescopes• Prime focus• Less sensitive to imperfections (due to longer wavelength); can be made very large
3.4 Radio Astronomy
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Largest radio telescope: 300-m dish at Arecibo
3.4 Radio Astronomy
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Longer wavelength means poorer angular resolution.Advantages of radio astronomy:• Can observe 24 hours a day.• Clouds, rain, and snow don’t interfere.• Observations at an entirely different frequency; get totally different information.
3.4 Radio Astronomy
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Interferometry:• Combines information from several widely spread radio telescopes as if it came from a single dish.• Resolution will be that of dish whose diameter = largest separation between dishes.
3.4 Radio Astronomy
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3.4 Radio Astronomy
Interferometry requires preserving the phase relationship between waves over the distance between individual telescopes.
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Can get radio images whose resolution is close to optical.
3.4 Radio Astronomy
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3.4 Radio Astronomy
Interferometry can also be done with visible light, but much harder due to shorter wavelengths.
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Infrared radiation can image where visible radiation is blocked; generally can use optical telescope mirrors and lenses.
3.5 Other Astronomies
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Infrared telescopes can also be in space or flown on balloons.
3.5 Other Astronomies
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Ultraviolet images(a)The Cygnus loop supernova remnant
(b) M81
3.5 Other Astronomies
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X rays and gamma rays will not reflect off mirrors as other wavelengths do; need new techniques.X rays will reflect at a very shallow angle, and can therefore be focused.
3.5 Other Astronomies
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X-ray image of supernova remnant Cassiopeia A
3.5 Other Astronomies
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Gamma rays cannot be focused at all; images are therefore somewhat coarser.
3.5 Other Astronomies
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Much can be learned from observing the same astronomical object at many wavelengths. Here, the Milky Way.
3.5 Other Astronomies
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• Refracting telescopes make images with a lens.
• Reflecting telescopes make images with a mirror.
• Modern research telescopes are all reflectors.
• CCDs are used for data collection.
• Data can be formed into image, analyzed spectroscopically, or used to measure intensity.
• Large telescopes gather much more light, allowing study of very faint sources.
• Large telescopes also have better resolution.
Summary of Chapter 3
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• Resolution of ground-based optical telescopes is limited by atmospheric effects.
• Resolution of radio or space-based telescopes is limited by diffraction.
• Active and adaptive optics can minimize atmospheric effects.
• Radio telescopes need large collection area; diffraction is limited.
• Interferometry can greatly improve resolution.
Summary of Chapter 3, cont.
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• Infrared and ultraviolet telescopes are similar to optical.
• Ultraviolet telescopes must be above atmosphere.
• X rays can be focused, but very differently than visible light.
• Gamma rays can be detected but not imaged.
Summary of Chapter 3, cont.