Two Fundamental Properties of a Telescope
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1 Two Fundamental Properties of a Telescope 1. Angular Resolution smallest angle which can be seen = 1.22 / D 2. Light-Collecting Area The telescope is a photon bucket A = (D/2)2 D A
2 Parts of the Human Eye pupil allows light to enter the eye lens focuses light to create an image retina detects the light and generates signals which are sent to the brain A camera works in the same way where the shutter acts like the pupil and the film or CCD acts like the retina!
3 Lenses bend Light Focus to bend all light waves coming from the same direction to a single point Light rays which come from different directions converge at different points to form an image.
4 Telescope Types Refractor focuses light using lenses Reflector focuses light using mirrors used exclusively in professional astronomy today
5 A refracting telescope uses a lens to concentrate incoming light Similar to a magnifying glass
6 Refracting telescopes have drawbacks Spherical aberration
7 Too spherical
8
9 Refracting telescopes have drawbacks Spherical aberration Chromatic aberration
10 Special achromatic compound lenses and lens coatings can often fix this aberration
11 Refracting telescopes have drawbacks Spherical aberration Chromatic aberration Sagging due to gravity distorting the lens Unwanted refractions opaque to certain wavelengths of light
12 Refractor Yerkes 40-inch telescope; largest refractor in the world
13 Reflector Gemini 8-m Telescope, Mauna Kea, Hawaii
14 Reflectors MMT Mt. Hopkins, AZ SUBARU Mauna Kea, HI
15 Reflecting telescopes use mirrors to concentrate incoming starlight
16 Newtonian Focus Prime Focus Cassegrain focus coude focus
17 Astronomer s face two major obstacles in observing the skies Light Pollution from Cities
18 Tucson, Arizona in 1959 and 1980
19 Astronomer s face two major obstacles in observing the skies Light Pollution from Cities Effects of Twinkling from Earth s atmosphere
20 Rapid changes in the density of Earth s atmosphere cause passing starlight to quickly change direction, making stars appear to twinkle.
21 Irregularities in the atmosphere s density cause the light to not arrive at the telescope as plane parrallel waves. Atmosphere Lens
22 Haleakalä Observatory, Maui (Faulkes Telescope North)
23 Advanced technology is spawning a new generation of equipment to view the universe CCDs (charge-coupled devices) Large telescopes on remote mountain tops Maunakea Cerro Pachon in Chile Orbiting space observatories Adaptive Optics to counteract the blurring of Earth s atmosphere
24 Adaptive Optics (AO) It is possible to de-twinkle a star. The wavefronts of a star s light rays are deformed by the atmosphere. By monitoring the distortions of the light from a nearby bright star (or a laser): a computer can deform the secondary mirror in the opposite way. the wavefronts, when reflected, are restored to their original state. Angular resolution improves. These two stars are separated by 0.38 Without AO, we see only one star. AO mirror off AO mirror on
25 A.O. Movie ao-animation.mov
26 Instruments in the Focal Plane How do astronomers use the light collected by a telescope? 1. Imaging use a camera to take pictures (images) Photometry measure total amount of light from an object 2. Spectroscopy use a spectrograph to separate the light into its different wavelengths (colors)
27 Filters are placed in front of a camera to allow only certain colors to be imaged Single color images are superimposed to form true color images. Imaging
28 A little color theory:
29 So why do TV s use RGB? Shouldn t they use RYB?
30 Spectroscopy The spectrograph reflects light off a grating: a finely ruled, smooth surface. Light interferes with itself and disperses into colors. This spectrum is recorded by a CCD detector.
31 Blocking the Aperture
32 Based on the idea of filling the aperture of a camera: Interferometry
33 kbk
34 Based on the idea of filling the aperture of a camera: Interferometry
35 Green Bank Interferometer 2004 Pearson Education Inc., publishing
36 The Very Large Array (VLA)
37 Traffic Jam, VLA Style
38
39
40
41 VLA Synthesized Aperture Synthesized aperture in a few minutes, as seen by the radio source Composed of 351 pairs of antennas
42 Synthesized Aperture 1 hour Synthesized aperture after 1 hr of Earth rotation Each pair fills in more of the aperture
43 Synthesized Aperture 10 Synthesized aperture after 10 hrs of Earth rotation Aperture is filled in Very high fidelity imaging hours
44 Radio Galaxy Cygnus A: Pre-VLA
45 Cygnus A Imaged by the VLA
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