Astronomy 114. Lecture 26: Telescopes. Martin D. Weinberg. UMass/Astronomy Department
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1 Astronomy 114 Lecture 26: Telescopes Martin D. Weinberg UMass/Astronomy Department A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 1/17
2 Announcements Quiz #2: we re aiming for this coming Friday... A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 2/17
3 Announcements Quiz #2: we re aiming for this coming Friday... Today: Optics and Telescopes Optics and Telescopes, Chap. 6 Tomorrow: Galaxies Galaxies, Chap. 26 A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 2/17
4 Telescopes What is a telescope? Collects light Focuses (concentrates) the photons onto a dectector Goals for telescopes Make sensitive observations distant objects Make BIG telescopes Resolve small details on the sky distant or nearby objects Angular resolution A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 3/17
5 Types of telescopes Refracting Focuses light through a lens. Examples: Camera lens Magnifying glass or eye glasses Reflecting Focuses light by reflecting light and changing its path in a coordinated way Examples: shaving or make-up mirror A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 4/17
6 Refraction (1/2) A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 5/17
7 Refraction (1/2) Demo A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 5/17
8 Refraction (1/2) A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 5/17
9 Refraction (2/2) Parallel light rays from a distant point come together at a focus point. Parallel rays from another distant point come together at a different focus point in the same plane ("focal plane"). A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 6/17
10 Refraction (2/2) Parallel light rays from a distant point come together at a focus point. Parallel rays from another distant point come together at a different focus point in the same plane ("focal plane"). A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 6/17
11 Refraction (2/2) A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 6/17
12 Refraction (2/2) Magnification = Focal length of objective Focal length of eyepice A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 7/17
13 Refraction (2/2) Magnification = Focal length of objective Focal length of eyepice Focal length of objective Focal ratio = Diameter of objective Smaller f-ratio more light reaches focal plane A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 7/17
14 Refracting telescope Goal of objective lens is to collect as much light as possible Simple design, still used for small amateur telescopes Limitations: Bending depends on wavelength, focal point depends on color! Lens must be supported at edges. Heavy glass lens sags under its own weight, distorts optics. A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 8/17
15 Reflection Law of reflection A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 9/17
16 Reflection Use reflection to focus light. Invented by Newton. A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy 114 9/17
17 Reflecting telescope A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
18 Reflecting telescope Largest refracting telescopes: 1-m primary lens Largest reflecting telescopes: 8-10 m primary mirror Mirror usually polished glass with thin layer of aluminum Can support mirror from behind to prevent sagging Nearly all modern telescopes are reflectors A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
19 Angular resolution Angular resolution ability to see structure Limited by the wavelike properties of light Image of a point of light is spread by the edge of the objective mirror or lens A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
20 Angular resolution Angular resolution ability to see structure Limited by the wavelike properties of light Image of a point of light is spread by the edge of the objective mirror or lens A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
21 Angular resolution Angular resolution ability to see structure Limited by the wavelike properties of light Image of a point of light is spread by the edge of the objective mirror or lens A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
22 Angular resolution Angular resolution ability to see structure Limited by the wavelike properties of light Image of a point of light is spread by the edge of the objective mirror or lens Radius of disk: θ = 1.22λ/D radians Points closer in angle than this are merged Examples: Human eye (0.2 cm pupil): about 1 arc minute 10 cm (4-inch) telescope: about 1 arc second 2.4 m (HST) telescope: about 0.05 arc second 10 m (Keck) telescope: about 0.01 arc second A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
23 Atmospheric seeing Blurring by air currents in atmosphere usually smears images over several arc-seconds seeing Best sites: arc second Atmospheric seeing limits the angular resolution of ground-based optical telescopes Solutions: 1. Put telescope in Earth orbit (hard, $$$) 2. Adaptively bend mirror to compensate for atmospheric motions (hard, $$$) A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
24 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors Made of heavy metals Reflect the rays just a few degrees Mirrors are rotated parabolas and hyperbolas A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
25 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
26 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
27 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
28 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors Gamma-ray telescopes give up on focusing entirely Use coded aperture masks The pattern of shadows the mask creates can be reconstructed to form an image A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
29 X-ray and gamma-ray telescopes High-energies photons interact with most materials X-ray telescopes use ring-shaped "glancing" mirrors Gamma-ray telescopes give up on focusing entirely Use coded aperture masks The pattern of shadows the mask creates can be reconstructed to form an image Satellites and balloons... why? A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
30 Transmittance of the Earth s atmosphere A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
31 Detectors (1/3) First detector: human eye Use secondary lens ("eyepiece") to make converging rays parallel again Limitations: Short exposure time (1/30 second) Have to rely on observer s description or drawing A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
32 Detectors (2/3) Better: film or photographic plates Put in focal plane, so extended image forms on plate Incoming photons cause permanent chemical change Long exposure increased sensitivity Permanent record Inefficient: best emulsions miss 99% of incoming photons A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
33 Detectors (3/3) State of the art: electronic detectors (CCDs) Incoming photons knock electrons out of silicon Electrons counted electronically Excellent efficiency: up to 80% of incoming photons counted Digital data, easily analyzed by computers CCDs have revolutionized optical astronomy (since c. 1980) In digital cameras and camcorders A114: Lecture Apr 2007 Read: Ch. 6,26 Astronomy /17
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