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In order to collect as much light as possible from a distant object, the objective should be as large as possible. However, in order to have large lenses manufactured, there are obvious problems. For example, it is essential to have the same optical properties throughout the lenses. Otherwise, any internal bubbles will alter the refractive index in those regions. Furthermore, lenses such as achromatic lenses tend to suffer from a residual amount of chromatic aberration (ie. optically dispersive). To overcome these difficulties is to build a telescope using parabolic mirror by the Newtonian design. However, most of the world largest telescopes nowadays employ the Cassegrain design. The advantage of this design is the beam-spreading qualities of the secondary mirror, which means that the effective focal length is several times that of the primary mirror. This allows for relatively more compact, easily-engineered, cost efficient and larger telescopes compared to telescopes engineered with Newtonian Design. Back to Home

Telescope objective lensfocal length

(FIGURE 1) Rays paths in a astronomical telescope system: the length of the telescope, L, becomes sum of the focal lengths, L= f1 + f2.

Glass can be recycled over and over. Glass bottles and jars can easily be recycled to make new glass bottles and jars or used in industry as aggregate (building material) or sand.

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The myth that glass is actually a liquid comes from the fact that old windows in houses and churches (200–300 years old) are sometimes a little out of shape: thicker at the bottom than the top. This is actually due to the process of glass making in the past which led to the glass pane being thicker at one edge than the other. It was sensible to install the windows with the thick edge at the bottom. Sometimes a window can be found with the thick edge at the top of the window.

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By changing the proportions, and adding different ingredients, many kinds of glass can be made. Coloured glass is made by adding small amounts of metal oxides. For example, a blue colour is given by tiny amounts of cobalt oxide.

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An eyepieceis a device which acts on an object and presents its image to the eye a much larger angle. An objective is the lens closest to the object that forms the initial image in an optical system. In a telescope, the image formed by the objective lens is an intermediate image. Astronomical telescope in which the image is inverted, is one of the two principal types of the telescopes. Its primary function is to enlarge the retinal image of a distant object. In the illustration (Fig. 1)below, the object is at a infinite distance form the objective, so that the intermediate image is formed in its secondary focal plane, which also coincides with the primary focal plane of the eyepiece. Then the eyepiece forms a virtual inverted image of this intermediate object at infinity. Both object and resulting inverted image are at infinity in this configuration. Also because of this configuration, the field stop of the telescope must be place at the intermediate image. To focus on an object, the eyepiece adjusts, while the intermediate image is fixed. The inverted image is not a problem, as long as the scope is used for astronomical observations since most work is photographic. Fragments of space that are captivated by the telescopes, are not rendered inverted, given that space has no “upside or down”. This is showed below. (FIGURE 1) Rays paths in a astronomical telescope system: the length of the telescope, L, becomes sum of the focal lengths, L= f1 + f2.  Mathematical Properties of Telescope This can be done through the ray tracing using the transfer matrix so the system matrix becomes: The ray-transfer from a plane at a distance d in front of the objective lens, to a plane at a distance d behind the eyepiece lens, is now given by the transfer matrix: Then the matrix reduces to where =y’ y is the magnification (where y’ is the image height and y is the object height). But, in contrast to other imaging systems, we now have the same magnification: In order to collect as much light as possible from a distant object, the objective should be as large as possible. However, in order to have large lenses manufactured, there are obvious problems. For example, it is essential to have the same optical properties throughout the lenses. Otherwise, any internal bubbles will alter the refractive index in those regions. Furthermore, lenses such as achromatic lenses tend to suffer from a residual amount of chromatic aberration (ie. optically dispersive). To overcome these difficulties is to build a telescope using parabolic mirror by the Newtonian design. However, most of the world largest telescopes nowadays employ the Cassegrain design. The advantage of this design is the beam-spreading qualities of the secondary mirror, which means that the effective focal length is several times that of the primary mirror. This allows for relatively more compact, easily-engineered, cost efficient and larger telescopes compared to telescopes engineered with Newtonian Design. Back to Home

(FIGURE 1) Rays paths in a astronomical telescope system: the length of the telescope, L, becomes sum of the focal lengths, L= f1 + f2.  Mathematical Properties of Telescope This can be done through the ray tracing using the transfer matrix so the system matrix becomes: The ray-transfer from a plane at a distance d in front of the objective lens, to a plane at a distance d behind the eyepiece lens, is now given by the transfer matrix: Then the matrix reduces to where =y’ y is the magnification (where y’ is the image height and y is the object height). But, in contrast to other imaging systems, we now have the same magnification: In order to collect as much light as possible from a distant object, the objective should be as large as possible. However, in order to have large lenses manufactured, there are obvious problems. For example, it is essential to have the same optical properties throughout the lenses. Otherwise, any internal bubbles will alter the refractive index in those regions. Furthermore, lenses such as achromatic lenses tend to suffer from a residual amount of chromatic aberration (ie. optically dispersive). To overcome these difficulties is to build a telescope using parabolic mirror by the Newtonian design. However, most of the world largest telescopes nowadays employ the Cassegrain design. The advantage of this design is the beam-spreading qualities of the secondary mirror, which means that the effective focal length is several times that of the primary mirror. This allows for relatively more compact, easily-engineered, cost efficient and larger telescopes compared to telescopes engineered with Newtonian Design. Back to Home

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Mar 25, 2013 — Table of Contents · 1 Fast cameras (jitter) · 2 Ever-changing near-field diameter (inscribed, circumscribed, square versus round, cutoffs, etc.) ...

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Chromatic Dispersion (CD) ... Chromatic dispersion (CD) is a deterministic phenomenon that refers to the broadening effect experienced by optical pulses emitted ...

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LEICA DG VARIO-ELMAR lens for outstanding photographic performance throughout zoom ranges; Ultra telephoto zoom lens covering up to 1600 mm*2 for use in a ...

Glass is a hard material that can be made in many shapes. It is usually transparent, but it can also be made in colours. Glass is mainly made of silica; glass made of silica only is called silica glass.

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The ray-transfer from a plane at a distance d in front of the objective lens, to a plane at a distance d behind the eyepiece lens, is now given by the transfer matrix:

Not including the cylinder information could have quite an impact on how well you see with the glasses! Yes, it does matter!

This lens has 1,176 prisms and 24 bullseyes. At the center, the bullseyes work like a magnilying glass so that the light beam is even more powerful. The lens ...

Glass used to make windows and bottles is a specific type called soda-lime glass, composed of about 75% silicon dioxide (SiO2), sodium oxide (Na2O) from sodium carbonate (Na2CO3), calcium oxide, also called lime (CaO), and several minor additives.

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where =y’ y is the magnification (where y’ is the image height and y is the object height). But, in contrast to other imaging systems, we now have the same magnification:

Crystal glass is made by adding lead and zinc oxides. It is not actually a crystal because all glass is a non-crystalline solid. Crystal glass is called cut glass if it has been cut by hand: