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Courtesy of UIT Team/NASA Chapter 5 Telescopes Courtesy of ESO Windows to the Universe The Crab nebula as seen in visible light The Crab nebula as seen in ultraviolet © 2004 Jones and Bartlett Publishers 5-1 Refraction and Image Formation 1. Light travels in a straight line as long as it remains in the same medium (i.e., the material that transmits light). 2. Refraction is the bending of light as it crosses the boundary (interface) between two materials in which it travels at different speeds. © 2004 Jones and Bartlett Publishers Figure 5.02a: As a light beam crosses the interface between different media, it bends due to the change in the speed of propagation. © 2004 Jones and Bartlett Publishers 3. The amount of refraction is determined by two factors: (a) Relative speeds of light in the two materials (e.g., air and glass). (b) Angle between a light ray and the interface; the smaller the angle between a light ray and the interface, the more the light bends on passing through the interface. 4. Image is the visual counterpoint of an object, formed by refraction or reflection of light from the object. © 2004 Jones and Bartlett Publishers 5. Focal point (of a converging lens or mirror) is the point at which light from a very distant object converges after being refracted or reflected. 6. Focal length is the distance from the center of a lens or a mirror to its focal point. Figure 5.03: (a) A lens bends incoming rays of light toward a single point. (b) Light from different stars are focused into separate images. © 2004 Jones and Bartlett Publishers 5-2 The Refracting Telescope 1. Objective is the main light-gathering element— lens or mirror—of a telescope. It is also called the primary. 2. An eyepiece (which may be a combination of lenses) added just beyond the focal point of the telescope’s objective acts as a magnifier to enlarge the image. © 2004 Jones and Bartlett Publishers Chromatic Aberration 1. Dispersion is the separation of light into its various wavelengths upon refraction. 2. Chromatic aberration is a defect of optical systems that results in light of different colors being focused at different places. The resulting image will be fuzzy at the edges. 3. An achromatic lens (or achromat) is an optical element that has been corrected so that it is free of chromatic aberration. This is done by combining two or more lenses made of different kinds of glass. © 2004 Jones and Bartlett Publishers Figure 5.06a: Chromatic aberration © 2004 Jones and Bartlett Publishers 5-3 The Powers of a Telescope Angular Size and Magnifying Power 1. Angular size of an object is the angle between two lines drawn from the viewer to opposite sides of the object. 2. Magnifying power (or magnification) is the ratio of the angular size of an object when it is seen through the instrument to its angular size when seen with the naked eye. Magnifying power: M = fobjective/feyepiece © 2004 Jones and Bartlett Publishers 3. Long focal length eyepieces produce less magnification; short focal length eyepieces produce more magnification. 4. Field of view is the actual angular width of the scene viewed by an optical instrument. 5. As magnification increases the field of view decreases. © 2004 Jones and Bartlett Publishers Light-Gathering Power 1. Light-gathering power is a measure of the amount of light collected by an optical instrument. 2. Light-gathering power is related to the size of the objective, which is usually given as a diameter. Remember that the area of a circle is proportional to the (diameter)2. © 2004 Jones and Bartlett Publishers Resolving Power 1. Diffraction is the spreading of light upon passing the edge of an object. 2. Resolving power (or resolution) is the smallest angular separation detectable with an instrument. It is a measure of an instrument’s ability to see detail. 3. The resolving power of a human eye is about 1 arcminute (1/60 of a degree). A 15-cm (6-inch) telescope has a maximum resolving power of 1 arcsecond (1/3600 of a degree). © 2004 Jones and Bartlett Publishers 4. Astronomical seeing is the blurring and twinkling of the image of an astronomical light source caused by the Earth’s atmosphere. 5. Seeing is the best possible angular resolution that can be achieved. 6. Because of atmospheric turbulence (which causes the stars to twinkle), even the largest Earth-based telescopes have a practical resolving power of between 1 and 0.25 arcsecond. 7. Operating above the atmosphere, the Hubble Space Telescope has a resolving power of 0.1 arcsecond or better. © 2004 Jones and Bartlett Publishers Figure 5.11: M-13 is a cluster of more than 100,000 stars about 23,000 ly away orbiting the center of our Galaxy. Courtesy of Gemini Observatory and Canada-France-Hawaii Telescope/Coelum/Jean-Charles Cuillandre © 2004 Jones and Bartlett Publishers 5-4 The Reflecting Telescope 1. An inwardly curved—or concave—mirror can bring incoming light rays to a focus and is used to construct reflecting telescopes. 2. In the late 1660s, Isaac Newton invented a special focal arrangement for a reflecting telescope by placing a small flat mirror in front of the objective mirror to deflect light rays out to the eyepiece. © 2004 Jones and Bartlett Publishers Figure 5.12a: The focal point is defined as the point where incoming rays that are parallel to the axis of the mirror converge. © 2004 Jones and Bartlett Publishers Figure 5.12b: The Newtonian focal arrangement. © 2004 Jones and Bartlett Publishers 3. Reflectors can be made larger (and less expensively) than refractors because: (a) There are fewer surfaces to grind, polish, and configure correctly. (b) Reflecting mirrors do not exhibit chromatic aberration as do lenses. (c) Light doesn’t transmit through a mirror so imperfections in the glass are not critical. (d) Mirrors can be supported on their backs, thus minimizing shape deformations due to gravity; lenses must be supported along their rims. © 2004 Jones and Bartlett Publishers Large Optical Telescopes 1. A Newtonian focus reflecting telescope has a plane mirror mounted along the axis of the telescope so that the mirror intercepts the light from the objective mirror and reflects it to the side. 2. A Cassegrain focus reflecting telescope has a secondary convex mirror that reflects the light back through a hole in the center of the primary mirror. 3. Prime focus is the point in a telescope where the light from the objective is focused (i.e., the focal point of the objective). © 2004 Jones and Bartlett Publishers 4. The Coude design allows for large and heavy equipment to be set at the focal point, outside the main telescope tube; here light reflects off three mirrors before it exits. Figure 5.16 © 2004 Jones and Bartlett Publishers 5. For best viewing conditions large telescopes are located on top of mountains in dry, clear climates. Figure 5.17a: The four telescopes of the Very Large Telescope Courtesy of ESO - (The) European Organization for Astronomical Research in the Southern Hemisphere © 2004 Jones and Bartlett Publishers Active and Adaptive Optics 1. Active optics is a technology that relies on a system that monitors and changes the shape of a telescope’s objective to produce the best image. 2. Adaptive optics is a technique that improves image quality by reducing the effects of astronomical seeing. © 2004 Jones and Bartlett Publishers Telescope Accessories 1. Camera with photographic plates. 2. Charge-coupled device (CCD) is an electronic “film” that serves as a light detector. It works by collecting electrons excited into higher energy states when the detector is struck by incident photons. The data collected is formed into images by a computer. 3. Photometry is the measurement of light intensity from a source, either the total intensity or the intensity at each of various wavelengths. Early photometers were like a camera’s light meter; modern photometers use a CCD for greater speed and accuracy. © 2004 Jones and Bartlett Publishers 4. Spectral analysis uses a spectrometer—an instrument that separates electromagnetic radiation according to wavelength. A spectrograph is a visual record of the spectrum taken by a spectrometer. 5. A spectrometer uses a diffraction grating—a device that uses the wave properties of EM radiation to separate the radiation into its various wavelengths. © 2004 Jones and Bartlett Publishers 5-5 Radio Telescopes 1. Compared to visible light, radio waves from a star have less intensity; also, their longer wavelengths lead to images of smaller resolution. 2. For better resolution in detecting radio waves, very large dishes are required. • The dish surfaces do not have to be as smooth as glass mirrors. • Even though longer wavelengths diffract more when going through an opening, they don’t require as smooth a surface for reflection. © 2004 Jones and Bartlett Publishers Figure 5.20: The radio telescope near Arecibo, Puerto Rico, is the world's largest. The Arecibo Observatory is part of the National Astronomy and Ionosphere Center, which is operated by Cornell University under a cooperative agreement with the National Science Foundation © 2004 Jones and Bartlett Publishers Figure 5.22: A graph, a contour map, and a color-enhanced contour map from scans of a radio telescope © 2004 Jones and Bartlett Publishers Figure 5.23b: A Spitzer infrared telescope telescope view of Andromeda Galaxy. Courtesy of JPL-Caltech/K. Gordon (University of Arizona)/NASA © 2004 Jones and Bartlett Publishers Figure 5.23c: A radio image of Andromeda shows that most radio waves are emitted from its spiral arms and from its center. Courtesy of Max-Planck-Institut fur Radioastronomie, Bonn (R. Beck, E.M. Berkhuijsen and P. Hoernes) © 2004 Jones and Bartlett Publishers 5-6 Interferometry 1. Interferometry is a procedure that allows a number of telescopes to be used as one by taking into account the time at which individual waves from an object strike each telescope. 2. Interferometry is possible because extremely accurate atomic clocks allow for precise timing of the signals received by radio telescopes from a distant object. 3. The farther apart the telescopes, the better the resolution. The VLBA has a resolution of a fraction of a milliarcsecond, 10,000 times better than earth-bound optical telescopes. 4. Interferometry can also be employed with the newest optical telescopes, such as the VLT in Chile or CHARA on Mount Wilson. © 2004 Jones and Bartlett Publishers Figure 5.26: The Very Large Array radio telescopes Courtesy of NRAO/AUI © 2004 Jones and Bartlett Publishers Figure 5.25: Interferometry © 2004 Jones and Bartlett Publishers Figure 5.24: two small radio telescope dishes replace one big dish. © 2004 Jones and Bartlett Publishers 5-7 Detecting Other Electromagnetic Radiation 1. Near infrared—1200 nm to 40,000 nm—can be detected from high, dry mountain tops such as Mauna Kea in Hawaii; water vapor is the main absorber of infrared light. 2. Far infrared—greater than 40,000 nm—can be detected from aircraft (e.g., the SOFIA project, NASA’s Airborne Observatory). 3. Infrared telescopes must be cooled so heat (IR radiation) from the surroundings does not mask the signals received from space. 4. Ozone is the chief absorber of wavelengths shorter than about 400 nm. Ultraviolet, X-ray and gamma-ray telescopes must be located in space. © 2004 Jones and Bartlett Publishers Figure 5.27: Spitzer’s infrared image of the W5 star forming region compared to a visible-light picture of the same region Infrared, Courtesy of NASA/JPL-Caltech/L. Allen (Harvard-Smithsonian CfA); Visible, Courtesy of CIT, DSS © 2004 Jones and Bartlett Publishers Tools of Astronomy: The Hubble Space Telescope 1. HST is mainly an optical telescope, with a 2.4-m primary mirror, but is designed to observe across the spectrum from near infrared to near ultraviolet (115–2500 nm). 2. The HST, after a number of servicing missions including a successful repair in 1993, is now functioning at design specifications. Its successor is the James Webb Space Telescope, schedule to launch in 2011. © 2004 Jones and Bartlett Publishers © 2004 Jones and Bartlett Publishers