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64-482: The TPS-1 is a lightweight portable search radar using a cut-down parabolic antenna of the "orange peel" design with an off-axis feed and transmitting in the L-band between 1220 and 1280 megahertz (MHz). The initial versions were designed to break down into ten packages and then be assembled on-site, but a number of adaptations to large trucks and even school bus frames were made over the years. A crew of two could operate

128-608: A traveling plane wave , whose evolution in time can be described as simple translation of the field at a constant wave speed c {\displaystyle c} along the direction perpendicular to the wavefronts. Such a field can be written as F ( x → , t ) = G ( x → ⋅ n → − c t ) {\displaystyle F({\vec {x}},t)=G\left({\vec {x}}\cdot {\vec {n}}-ct\right)\,} where G ( u ) {\displaystyle G(u)}

192-426: A complex exponential plane wave . When the values of F {\displaystyle F} are vectors, the wave is said to be a longitudinal wave if the vectors are always collinear with the vector n → {\displaystyle {\vec {n}}} , and a transverse wave if they are always orthogonal (perpendicular) to it. Often the term "plane wave" refers specifically to

256-448: A circular dish or various other shapes to create different beam shapes. A metal screen reflects radio waves as effectively as a solid metal surface if its holes are smaller than one-tenth of a wavelength , so screen reflectors are often used to reduce weight and wind loads on the dish. To achieve the maximum gain , the shape of the dish needs to be accurate within a small fraction of a wavelength, around one sixteenth wavelength, to ensure

320-470: A coat of flat paint. The feed antenna at the reflector's focus is typically a low-gain type, such as a half-wave dipole or (more often) a small horn antenna called a feed horn . In more complex designs, such as the Cassegrain and Gregorian, a secondary reflector is used to direct the energy into the parabolic reflector from a feed antenna located away from the primary focal point. The feed antenna

384-476: A curved surface with the cross-sectional shape of a parabola , to direct the radio waves . The most common form is shaped like a dish and is popularly called a dish antenna or parabolic dish . The main advantage of a parabolic antenna is that it has high directivity . It functions similarly to a searchlight or flashlight reflector to direct radio waves in a narrow beam, or receive radio waves from one particular direction only. Parabolic antennas have some of

448-617: A function of one scalar parameter (the displacement d = x → ⋅ n → {\displaystyle d={\vec {x}}\cdot {\vec {n}}} ) with scalar or vector values, and S {\displaystyle S} is a scalar function of time. This representation is not unique, since the same field values are obtained if S {\displaystyle S} and G {\displaystyle G} are scaled by reciprocal factors. If | S ( t ) | {\displaystyle \left|S(t)\right|}

512-411: A large homogeneous region of space can be well approximated by plane waves when viewed over any part of that region that is sufficiently small compared to its distance from the source. That is the case, for example, of the light waves from a distant star that arrive at a telescope. A standing wave is a field whose value can be expressed as the product of two functions, one depending only on position,

576-412: A parabolic antenna is that a point source of radio waves at the focal point in front of a paraboloidal reflector of conductive material will be reflected into a collimated plane wave beam along the axis of the reflector. Conversely, an incoming plane wave parallel to the axis will be focused to a point at the focal point. A typical parabolic antenna consists of a metal parabolic reflector with

640-490: A radian). For a typical parabolic antenna, k is approximately 70. For a typical 2 meter satellite dish operating on C band (4 GHz), this formula gives a beamwidth of about 2.6°. For the Arecibo antenna at 2.4 GHz, the beamwidth was 0.028°. Since parabolic antennas can produce very narrow beams, aiming them can be a problem. Some parabolic dishes are equipped with a boresight so they can be aimed accurately at

704-476: A scalar or a vector, is called the amplitude of the wave; the scalar coefficient f {\displaystyle f} is its "spatial frequency"; and the scalar φ {\displaystyle \varphi } is its " phase shift ". A true plane wave cannot physically exist, because it would have to fill all space. Nevertheless, the plane wave model is important and widely used in physics. The waves emitted by any source with finite extent into

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768-490: A small feed antenna suspended in front of the reflector at its focus, pointed back toward the reflector. The reflector is a metallic surface formed into a paraboloid of revolution and usually truncated in a circular rim that forms the diameter of the antenna. In a transmitting antenna, radio frequency current from a transmitter is supplied through a transmission line cable to the feed antenna , which converts it into radio waves. The radio waves are emitted back toward

832-528: A uniform illumination of the primary, to maximize the gain. However, this results in a secondary that is no longer precisely hyperbolic (though it is still very close), so the constant phase property is lost. This phase error, however, can be compensated for by slightly tweaking the shape of the primary mirror. The result is a higher gain, or gain/spillover ratio, at the cost of surfaces that are trickier to fabricate and test. Other dish illumination patterns can also be synthesized, such as patterns with high taper at

896-935: A wave in a one-dimensional medium. Any local operator , linear or not, applied to a plane wave yields a plane wave. Any linear combination of plane waves with the same normal vector n → {\displaystyle {\vec {n}}} is also a plane wave. For a scalar plane wave in two or three dimensions, the gradient of the field is always collinear with the direction n → {\displaystyle {\vec {n}}} ; specifically, ∇ F ( x → , t ) = n → ∂ 1 G ( x → ⋅ n → , t ) {\displaystyle \nabla F({\vec {x}},t)={\vec {n}}\partial _{1}G({\vec {x}}\cdot {\vec {n}},t)} , where ∂ 1 G {\displaystyle \partial _{1}G}

960-505: A wavelength of 21 cm (1.42 GHz, a common radio astronomy frequency), yields an approximate maximum gain of 140,000 times or about 52 dBi ( decibels above the isotropic level). The largest parabolic dish antenna in the world is the Five-hundred-meter Aperture Spherical radio Telescope in southwest China, which has an effective aperture of about 300 meters. The gain of this dish at 3 GHz

1024-440: Is a unit-length vector , and G ( d , t ) {\displaystyle G(d,t)} is a function that gives the field's value as dependent on only two real parameters: the time t {\displaystyle t} , and the scalar-valued displacement d = x → ⋅ n → {\displaystyle d={\vec {x}}\cdot {\vec {n}}} of

1088-535: Is bounded in the time interval of interest (which is usually the case in physical contexts), S {\displaystyle S} and G {\displaystyle G} can be scaled so that the maximum value of | S ( t ) | {\displaystyle \left|S(t)\right|} is 1. Then | G ( x → ⋅ n → ) | {\displaystyle \left|G({\vec {x}}\cdot {\vec {n}})\right|} will be

1152-546: Is called the direction of propagation . For each displacement d {\displaystyle d} , the moving plane perpendicular to n → {\displaystyle {\vec {n}}} at distance d + c t {\displaystyle d+ct} from the origin is called a " wavefront ". This plane travels along the direction of propagation n → {\displaystyle {\vec {n}}} with velocity c {\displaystyle c} ; and

1216-477: Is connected to the associated radio-frequency (RF) transmitting or receiving equipment by means of a coaxial cable transmission line or waveguide . At the microwave frequencies used in many parabolic antennas, waveguide is required to conduct the microwaves between the feed antenna and transmitter or receiver. Because of the high cost of waveguide runs, in many parabolic antennas the RF front end electronics of

1280-623: Is constant through any plane that is perpendicular to a fixed direction in space. For any position x → {\displaystyle {\vec {x}}} in space and any time t {\displaystyle t} , the value of such a field can be written as F ( x → , t ) = G ( x → ⋅ n → , t ) , {\displaystyle F({\vec {x}},t)=G({\vec {x}}\cdot {\vec {n}},t),} where n → {\displaystyle {\vec {n}}}

1344-646: Is for radar antennas, which need to transmit a narrow beam of radio waves to locate objects like ships, airplanes , and guided missiles . They are also often used for weather detection. With the advent of home satellite television receivers, parabolic antennas have become a common feature of the landscapes of modern countries. The parabolic antenna was invented by German physicist Heinrich Hertz during his discovery of radio waves in 1887. He used cylindrical parabolic reflectors with spark-excited dipole antennas at their foci for both transmitting and receiving during his historic experiments. The operating principle of

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1408-460: Is measured by a parameter called cross polarization discrimination (XPD). In a transmitting antenna, XPD is the fraction of power from an antenna of one polarization radiated in the other polarization. For example, due to minor imperfections a dish with a vertically polarized feed antenna will radiate a small amount of its power in horizontal polarization; this fraction is the XPD. In a receiving antenna,

1472-529: Is now a function of a single real parameter u = d − c t {\displaystyle u=d-ct} , that describes the "profile" of the wave, namely the value of the field at time t = 0 {\displaystyle t=0} , for each displacement d = x → ⋅ n → {\displaystyle d={\vec {x}}\cdot {\vec {n}}} . In that case, n → {\displaystyle {\vec {n}}}

1536-435: Is roughly 90 million, or 80 dBi. Aperture efficiency e A is a catchall variable which accounts for various losses that reduce the gain of the antenna from the maximum that could be achieved with the given aperture. The major factors reducing the aperture efficiency in parabolic antennas are: For theoretical considerations of mutual interference (at frequencies between 2 and approximately 30 GHz; typically in

1600-402: Is the diameter of the antenna's aperture in meters, λ {\displaystyle \lambda } is the wavelength in meters, θ {\displaystyle \theta } is the angle in radians from the antenna's symmetry axis as shown in the figure, and J 1 {\displaystyle J_{1}} is the first-order Bessel function . Determining

1664-831: Is the partial derivative of G {\displaystyle G} with respect to the first argument. The divergence of a vector-valued plane wave depends only on the projection of the vector G ( d , t ) {\displaystyle G(d,t)} in the direction n → {\displaystyle {\vec {n}}} . Specifically, ∇ ⋅ F → ( x → , t ) = n → ⋅ ∂ 1 G ( x → ⋅ n → , t ) {\displaystyle \nabla \cdot {\vec {F}}({\vec {x}},t)\;=\;{\vec {n}}\cdot \partial _{1}G({\vec {x}}\cdot {\vec {n}},t)} In particular,

1728-535: The half-power beam width (HPBW), which is the angular separation between the points on the antenna radiation pattern at which the power drops to one-half (-3 dB) its maximum value. For parabolic antennas, the HPBW θ is given by: where k is a factor which varies slightly depending on the shape of the reflector and the feed illumination pattern. For an ideal uniformly illuminated parabolic reflector and θ in degrees, k would be 57.3 (the number of degrees in

1792-543: The Fixed Satellite Service ) where specific antenna performance has not been defined, a reference antenna based on Recommendation ITU-R S.465 is used to calculate the interference, which will include the likely sidelobes for off-axis effects. In parabolic antennas, virtually all the power radiated is concentrated in a narrow main lobe along the antenna's axis. The residual power is radiated in sidelobes , usually much smaller, in other directions. Since

1856-529: The Telstar satellite. The Cassegrain antenna was developed in Japan in 1963 by NTT , KDDI , and Mitsubishi Electric . The Voyager 1 spacecraft launched in 1977 is currently 24.2 billion kilometers from Earth, the furthest manmade object in space, and it's 3.7 meter S and X-band Cassegrain antenna (see picture above) is still able to communicate with ground stations. The advent of computer design tools in

1920-528: The 1930s in investigations of UHF transmission from his boat in the Mediterranean. In 1931, a 1.7 GHz microwave relay telephone link across the English Channel was demonstrated using 3.0-meter (10 ft) diameter dishes. The first large parabolic antenna, a 9 m dish, was built in 1937 by pioneering radio astronomer Grote Reber in his backyard, and the sky survey he did with it

1984-425: The 1970s—such as NEC , capable of calculating the radiation pattern of parabolic antennas—has led to the development of sophisticated asymmetric, multi-reflector and multi-feed designs in recent years. [REDACTED] Media related to Parabolic antennas at Wikimedia Commons Plane wave In physics , a plane wave is a special case of a wave or field : a physical quantity whose value, at any moment,

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2048-466: The Cassegrain and Gregorian antennas, the presence of two reflecting surfaces in the signal path offers additional possibilities for improving performance. When the highest performance is required, a technique called dual reflector shaping may be used. This involves changing the shape of the sub-reflector to direct more signal power to outer areas of the dish, to map the known pattern of the feed into

2112-410: The XPD is the ratio of signal power received of the opposite polarization to power received in the same antenna of the correct polarization, when the antenna is illuminated by two orthogonally polarized radio waves of equal power. If the antenna system has inadequate XPD, cross polarization interference cancelling (XPIC) digital signal processing algorithms can often be used to decrease crosstalk. In

2176-530: The antenna (all of it except the feed antenna) is nonresonant , so it can function over a wide range of frequencies (i.e. a wide bandwidth ). All that is necessary to change the frequency of operation is to replace the feed antenna with one that operates at the desired frequency. Some parabolic antennas transmit or receive at multiple frequencies by having several feed antennas mounted at the focal point, close together. Parabolic antennas are distinguished by their shapes: Parabolic antennas are also classified by

2240-709: The aperture is large, the angle θ 0 {\displaystyle \theta _{0}} is very small, so arcsin ⁡ ( x ) {\displaystyle \arcsin(x)} is approximately equal to x {\displaystyle x} . This gives the common beamwidth formulas, θ 0 ≈ 1.22 λ D (in radians) = 70 λ D (in degrees) {\displaystyle \theta _{0}\approx {\frac {1.22\lambda }{D}}\,{\text{(in radians)}}={\frac {70\lambda }{D}}\,{\text{(in degrees)}}} The idea of using parabolic reflectors for radio antennas

2304-406: The dish by the feed antenna and reflect off the dish into a parallel beam. In a receiving antenna the incoming radio waves bounce off the dish and are focused to a point at the feed antenna, which converts them into electric currents which travel through a transmission line to the radio receiver . The reflector can be constructed from sheet metal, a metal screen, or a wire grill, and can be either

2368-465: The dish edge for ultra-low spillover sidelobes , and patterns with a central "hole" to reduce feed shadowing. The directive qualities of an antenna are measured by a dimensionless parameter called its gain , which is the ratio of the power received by the antenna from a source along its beam axis to the power received by a hypothetical isotropic antenna . The gain of a parabolic antenna is: where: It can be seen that, as with any aperture antenna ,

2432-436: The edges. However, practical feed antennas have radiation patterns that drop off gradually at the edges, so the feed antenna is a compromise between acceptably low spillover and adequate illumination. For most front feed horns, optimum illumination is achieved when the power radiated by the feed horn is 10 dB less at the dish edge than its maximum value at the center of the dish. The pattern of electric and magnetic fields at

2496-534: The electric field pattern E ( θ ) {\displaystyle E(\theta )} , E ( θ ) = 2 λ π D J 1 [ ( π D / λ ) sin ⁡ θ ] sin ⁡ θ {\displaystyle E(\theta )={\frac {2\lambda }{\pi D}}{\frac {J_{1}[(\pi D/\lambda )\sin \theta ]}{\sin \theta }}} where D {\displaystyle D}

2560-425: The feed is horizontal ( horizontal polarization ) the antenna will suffer a severe loss of gain. To increase the data rate, some parabolic antennas transmit two separate radio channels on the same frequency with orthogonal polarizations, using separate feed antennas; this is called a dual polarization antenna . For example, satellite television signals are transmitted from the satellite on two separate channels at

2624-630: The first nulls of the radiation pattern gives the beamwidth θ 0 {\displaystyle \theta _{0}} . The term J 1 ( x ) = 0 {\displaystyle J_{1}(x)=0} whenever x = 3.83 {\displaystyle x=3.83} . Thus, θ 0 = arcsin ⁡ 3.83 λ π D = arcsin ⁡ 1.22 λ D {\displaystyle \theta _{0}=\arcsin {\frac {3.83\lambda }{\pi D}}=\arcsin {\frac {1.22\lambda }{D}}} . When

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2688-428: The gain and increasing the backlobes , possibly causing interference or (in receiving antennas) increasing susceptibility to ground noise. However, maximum gain is only achieved when the dish is uniformly "illuminated" with a constant field strength to its edges. Therefore, the ideal radiation pattern of a feed antenna would be a constant field strength throughout the solid angle of the dish, dropping abruptly to zero at

2752-427: The grill elements. This type is often used in radar antennas. Combined with a linearly polarized feed horn , it helps filter out noise in the receiver and reduces false returns. A shiny metal parabolic reflector can also focus the sun's rays. Since most dishes could concentrate enough solar energy on the feed structure to severely overheat it if they happened to be pointed at the sun, solid reflectors are always given

2816-864: The highest gains , meaning that they can produce the narrowest beamwidths , of any antenna type. In order to achieve narrow beamwidths, the parabolic reflector must be much larger than the wavelength of the radio waves used, so parabolic antennas are used in the high frequency part of the radio spectrum , at UHF and microwave ( SHF ) frequencies, at which the wavelengths are small enough that conveniently sized reflectors can be used. Parabolic antennas are used as high-gain antennas for point-to-point communications , in applications such as microwave relay links that carry telephone and television signals between nearby cities, wireless WAN/LAN links for data communications, satellite communications , and spacecraft communication antennas. They are also used in radio telescopes . The other large use of parabolic antennas

2880-423: The larger the aperture is, compared to the wavelength , the higher the gain. The gain increases with the square of the ratio of aperture width to wavelength, so large parabolic antennas, such as those used for spacecraft communication and radio telescopes , can have extremely high gain. Applying the above formula to the 25-meter-diameter antennas often used in radio telescope arrays and satellite ground antennas at

2944-500: The maximum field magnitude seen at the point x → {\displaystyle {\vec {x}}} . A plane wave can be studied by ignoring the directions perpendicular to the direction vector n → {\displaystyle {\vec {n}}} ; that is, by considering the function G ( z , t ) = F ( z n → , t ) {\displaystyle G(z,t)=F(z{\vec {n}},t)} as

3008-508: The mouth of a parabolic antenna is simply a scaled-up image of the fields radiated by the feed antenna, so the polarization is determined by the feed antenna. In order to achieve maximum gain, both feed antennas (transmitting and receiving) must have the same polarization. For example, a vertical dipole feed antenna will radiate a beam of radio waves with their electric field vertical, called vertical polarization . The receiving feed antenna must also have vertical polarization to receive them; if

3072-423: The other antenna. There is an inverse relation between gain and beam width. By combining the beamwidth equation with the gain equation, the relation is: The radiation from a large paraboloid with uniform illuminated aperture is essentially equivalent to that from a circular aperture of the same diameter D {\displaystyle D} in an infinite metal plate with a uniform plane wave incident on

3136-626: The other for receiving, Hertz demonstrated the existence of radio waves which had been predicted by James Clerk Maxwell some 22 years earlier. However, the early development of radio was limited to lower frequencies at which parabolic antennas were unsuitable, and they were not widely used until World War II , when microwave frequencies began to be employed. After World War I when short waves began to be used, interest grew in directional antennas , both to increase range and make radio transmissions more secure from interception. Italian radio pioneer Guglielmo Marconi used parabolic reflectors during

3200-399: The other only on time. A plane standing wave , in particular, can be expressed as F ( x → , t ) = G ( x → ⋅ n → ) S ( t ) {\displaystyle F({\vec {x}},t)=G({\vec {x}}\cdot {\vec {n}})\,S(t)} where G {\displaystyle G} is

3264-1788: The plate. The radiation-field pattern can be calculated by applying Huygens' principle in a similar way to a rectangular aperture. The electric field pattern can be found by evaluating the Fraunhofer diffraction integral over the circular aperture. It can also be determined through Fresnel zone equations . E = ∫ ∫ A r 1 e j ( ω t − β r 1 ) d S = ∫ ∫ e 2 π i ( l x + m y ) / λ d S {\displaystyle E=\int \int {\frac {A}{r_{1}}}e^{j(\omega t-\beta r_{1})}dS=\int \int e^{2\pi i(lx+my)/\lambda }dS} where β = ω / c = 2 π / λ {\displaystyle \beta =\omega /c=2\pi /\lambda } . Using polar coordinates, x = ρ ⋅ cos ⁡ θ {\displaystyle x=\rho \cdot \cos \theta } and y = ρ ⋅ sin ⁡ θ {\displaystyle y=\rho \cdot \sin \theta } . Taking account of symmetry, E = ∫ 0 2 π d θ ∫ 0 ρ 0 e 2 π i ρ cos ⁡ θ l / λ ρ d ρ {\displaystyle E=\int \limits _{0}^{2\pi }d\theta \int \limits _{0}^{\rho _{0}}e^{2\pi i\rho \cos \theta l/\lambda }\rho d\rho } and using first-order Bessel function gives

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3328-516: The point x → {\displaystyle {\vec {x}}} along the direction n → {\displaystyle {\vec {n}}} . The displacement is constant over each plane perpendicular to n → {\displaystyle {\vec {n}}} . The values of the field F {\displaystyle F} may be scalars, vectors, or any other physical or mathematical quantity. They can be complex numbers , as in

3392-526: The radar. The 1B model could detect bombers at 10,000 feet at a distance of 120 nautical miles. Versions B through G differed primarily in the antenna pattern, providing better vertical range, but were electrically identical. TPS-1s were used to defend many beach-heads in the Pacific during the war and were among the first portable radar units to go into operation following the invasions of Iwo Jima and Okinawa . These units saw considerable postwar service. It

3456-409: The receiver is located at the feed antenna, and the received signal is converted to a lower intermediate frequency (IF) so it can be conducted to the receiver through cheaper coaxial cable . This is called a low-noise block downconverter . Similarly, in transmitting dishes, the microwave transmitter may be located at the feed point. An advantage of parabolic antennas is that most of the structure of

3520-406: The reflector aperture of parabolic antennas is much larger than the wavelength, diffraction usually causes many narrow sidelobes, so the sidelobe pattern is complex. There is also usually a backlobe , in the opposite direction to the main lobe, due to the spillover radiation from the feed antenna that misses the reflector. The angular width of the beam radiated by high-gain antennas is measured by

3584-473: The same frequency using right and left circular polarization . In a home satellite dish , these are received by two small monopole antennas in the feed horn , oriented at right angles. Each antenna is connected to a separate receiver. If the signal from one polarization channel is received by the oppositely polarized antenna, it will cause crosstalk that degrades the signal-to-noise ratio . The ability of an antenna to keep these orthogonal channels separate

3648-409: The type of feed , that is, how the radio waves are supplied to the antenna: The radiation pattern of the feed antenna has to be tailored to the shape of the dish, because it has a strong influence on the aperture efficiency , which determines the antenna gain (see gain section below). Radiation from the feed that falls outside the edge of the dish is called spillover and is wasted, reducing

3712-778: The value of the field is then the same, and constant in time, at every one of its points. The term is also used, even more specifically, to mean a "monochromatic" or sinusoidal plane wave : a travelling plane wave whose profile G ( u ) {\displaystyle G(u)} is a sinusoidal function. That is, F ( x → , t ) = A sin ⁡ ( 2 π f ( x → ⋅ n → − c t ) + φ ) {\displaystyle F({\vec {x}},t)=A\sin \left(2\pi f({\vec {x}}\cdot {\vec {n}}-ct)+\varphi \right)} The parameter A {\displaystyle A} , which may be

3776-409: The waves from different parts of the antenna arrive at the focus in phase . Large dishes often require a supporting truss structure behind them to provide the required stiffness. A reflector made of a grill of parallel wires or bars oriented in one direction acts as a polarizing filter as well as a reflector. It only reflects linearly polarized radio waves, with the electric field parallel to

3840-452: The world's first parabolic reflector antenna in 1888. The antenna was a cylindrical parabolic reflector made of zinc sheet metal supported by a wooden frame, and had a spark-gap excited 26 cm dipole as a feed antenna along the focal line. Its aperture was 2 meters high by 1.2 meters wide, with a focal length of 0.12 meters, and was used at an operating frequency of about 450 MHz. With two such antennas, one used for transmitting and

3904-470: Was completed in 1962—is currently the world's largest fully steerable parabolic dish. During the 1960s, dish antennas became widely used in terrestrial microwave relay communication networks, which carried telephone calls and television programs across continents. The first parabolic antenna used for satellite communications was constructed in 1962 at Goonhilly in Cornwall , England, to communicate with

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3968-546: Was one of the events that founded the field of radio astronomy . The development of radar during World War II provided a great impetus to parabolic antenna research. This led to the evolution of shaped-beam antennas, in which the curve of the reflector is different in the vertical and horizontal directions, tailored to produce a beam with a particular shape. After the war, very large parabolic dishes were built as radio telescopes . The 100-meter Green Bank Radio Telescope at Green Bank, West Virginia —the first version of which

4032-413: Was taken from optics , where the power of a parabolic mirror to focus light into a beam has been known since classical antiquity . The designs of some specific types of parabolic antenna, such as the Cassegrain and Gregorian , come from similarly named analogous types of reflecting telescope , which were invented by astronomers during the 15th century. German physicist Heinrich Hertz constructed

4096-513: Was used in the temporary Lashup Radar Network beginning in 1948. The AN/TPS-1D was the main component of the AN/GSS-1 Electronic Search Central system used with Nike missile systems. [REDACTED]  This article incorporates public domain material from the Air Force Historical Research Agency Parabolic antenna A parabolic antenna is an antenna that uses a parabolic reflector ,

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