reflecting telescope oor Masedonies
reflecting telescope
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A telescope which produces a magnified image by reflecting light through a series of mirrors housed in a tube, using a large curved mirror to gather the light and one or more additional mirrors to transmit the light to an eyepiece.
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telescopes that reflect light with a combination of mirrors
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In 1762, Lomonosov presented an improved design of a reflecting telescope to the Russian Academy of Sciences forum.
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Reflecting telescopes, just like any other optical system, do not produce "perfect" images.
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Since reflecting telescopes use mirrors, the design is sometimes referred to as a "catoptric" telescope.
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Prior to Foucault's publication of his findings, the testing of reflecting telescope mirrors was a "hit or miss" proposition.
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Although reflecting telescopes produce other types of optical aberrations, it is a design that allows for very large diameter objectives.
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Since I was interested in astronomy, I undertook building a large reflecting telescope with an eight-inch-[20 cm]diameter mirror.
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To avoid this problem most reflecting telescopes use parabolic shaped mirrors, a shape that can focus all the light to a common focus.
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Since 1976 the largest reflecting telescope in the world has been the 236-inch telescope at the Zelenchukskaya Astrophysical Observatory in the Caucasus, Russia.
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In contrast, a mirror can be supported by the whole side opposite its reflecting face, allowing for reflecting telescope designs that can overcome gravitational sag.
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Reflecting telescopes come in many design variations and may employ extra optical elements to improve image quality or place the image in a mechanically advantageous position.
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A reflecting telescope (also called a reflector) is a telescope that uses a single or a combination of curved mirrors that reflect light and form an image.
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Since crafting large lenses is much more difficult than crafting large mirrors, most modern telescopes are reflecting telescopes, that is, telescopes that use a primary mirror rather than an objective lens.
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There are reflecting telescope designs that use modified mirror surfaces (such as the Ritchey–Chrétien telescope) or some form of correcting lens (such as catadioptric telescopes) that correct some of these aberrations.
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The reflecting telescope was invented in the 17th century, by Isaac Newton, as an alternative to the refracting telescope which, at that time, was a design that suffered from severe chromatic aberration.
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The late 20th century has seen the development of adaptive optics and lucky imaging to overcome the problems of seeing, and reflecting telescopes are ubiquitous on space telescopes and many types of spacecraft imaging devices.
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In April 1992, however, the new Keck* reflecting optical telescope was completed on Mauna Kea in Hawaii.
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Because the primary mirror focuses light to a common point in front of its own reflecting surface almost all reflecting telescope designs have a secondary mirror, film holder, or detector near that focal point partially obstructing the light from reaching the primary mirror.
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The need to image objects at distances up to infinity, view them at different wavelengths of light, along with the requirement to have some way to view the image the primary mirror produces, means there is always some compromise in a reflecting telescope's optical design.
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Many of the advances in reflecting telescopes included the perfection of parabolic mirror fabrication in the 18th century, silver coated glass mirrors in the 19th century, long-lasting aluminum coatings in the 20th century, segmented mirrors to allow larger diameters, and active optics to compensate for gravitational deformation.
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The potential advantages of using parabolic mirrors (primarily a reduction of spherical aberration with elimination of chromatic aberration) led to several proposed designs for reflecting telescopes, the most notable of which was published in 1663 by James Gregory and came to be called the Gregorian telescope, but no working models were built.
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The OSO and OAO missions demonstrated the important role space-based observations could play in astronomy, and in 1968, NASA developed firm plans for a space-based reflecting telescope with a mirror 3 m (9.8 ft) in diameter, known provisionally as the Large Orbiting Telescope or Large Space Telescope (LST), with a launch slated for 1979.
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Albedo features are areas of markedly different reflectivity, as seen by telescopic observation.
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Stephan made this discovery with the first telescope equipped with a reflection coated mirror.
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He preferred iron sights over telescopic sights, as they enable a sniper to present a smaller target for the enemy (a sniper must raise his head a few centimeters higher when using a telescopic sight), and can be relied on even in extreme cold (unlike telescopic sights, which tend to cloud up in cold weather), and are easier to conceal (sunlight can reflect off a telescopic sight's lenses and reveal the sniper's position).
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A flat secondary mirror reflects the light to a focal plane at the side of the top of the telescope tube.
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