131 Sentences With "dish antenna" | Random Sentence Generator

A dish antenna could fit easily into a small van.

Practically every house, including Mr. Roth's, seems to have a TV dish antenna.

Beside the tent, a ten-foot-tall dish antenna is trying to establish a connection with the plane.

A skinny Boxer mix pants from the shadow of the dish antenna where it's been tied up nearby.

This dish antenna rises seven stories above an ancient seabed in the Karoo, a remote semidesert in South Africa.

From there, a radio connection is made from a dish antenna 22019 feet in diameter, sheltered by an egg-shaped dome the size of a cottage.

His company has built phased array radars that steer the radar beam electronically — faster than a traditional dish antenna — in three locations: Alaska, Texas and New Zealand.

They were able to get its location by taking advantage of the fact that the FRB traveled a slightly different distance to reach each dish antenna, arriving at a slightly different time.

The largest scientific structure ever powers up in Africa Towering above an ancient seabed in the Karoo—a remote semidesert in South Africa—is a seven-story dish antenna that will soon begin scanning the universe for its deepest secrets.

This might be a vegetable garden for the inhabitants of the lit building in the background, but every element in this painting asks to be read allegorically: the silhouetted African figure is a representative of the primordial; the sprinklers and garden are modern, regulated production; the satellite dish antenna on the back building represent the technically sophisticated people using these resources; and the small water bottle in the foreground speaks to our selfish, personalized, wasteful, yet aesthetically pleasing habits of nourishment — which ultimately are unsustainable.

Diplexers are also used in the home to allow a direct broadcast satellite TV dish antenna and a terrestrial TV antenna (local broadcast channels) to share one coaxial cable. The dish antenna occupies the high frequencies (typically 950 to 1450 MHz), and the TV antenna uses lower television channel frequencies (typically 50 to 870 MHz). In addition, the satellite also gets a DC to low frequency band to power the dish's block converter and select the dish antenna polarization (e.g., voltage signaling or DiSEqC).

Another, third division, is the Kalyazin Radio Astronomy Observatory, at . It has a dish antenna to the east of Kalyazin.

Quick Reaction Satellite Antenna Group (QRSAG) antenna, while the outlying spoke terminals rely on an 8 ft. parabolic dish antenna.

The lighthouse is two storied, with accommodation for the lighthouse keepers and a dish antenna. The reef is named after the East Indiaman .

One of the ten dish-antenna radiotelescope systems of the Very Long Baseline Array is located on a sublease within the Owens Valley observatory.

This included the installation of the satellite dish antenna off the coast of Vietnam and was performed by the ship-fitters in the Engineering Department.

SPANDAR's sensitivity with its dish antenna can detect small changes in the refractive index of air caused by sea breeze fronts, gust fronts, and various forms of clear air turbulence.

On 23 July 2013, the German Aerospace Center scientists pointed their 30-meter dish antenna at Weilheim towards the satellite and found that it was already transmitting a signal in the L5 frequency band.

The Haystack Auxiliary Radar (HAX) is Ku-band system with a dish antenna. It was constructed in 1993 to augment the LSSC imaging and data collections space debris. It contributes data to the SSN.

The Millstone Hill Steerable Antenna, or MISA, is a fully steerable dish antenna, in diameter, designed by the Stanford Research Institute (SRI) in 1959. It is currently located at MIT Haystack Observatory in Westford, Massachusetts.

Other systems currently used for space surveillance that operate in beam-park mode include the multistatic EISCAT incoherent scatter radar system and the Medicina Radio Observatory's Northern Cross Radio Telescope and 32 m parabolic dish antenna.

The Venera 15 and 16 spacecraft were identical and were based on modifications to the orbiter portions of the Venera 9 and Venera 14 probes. Each spacecraft consisted of a 5 m long cylinder with a 0.6 m diameter, 1.4 m tall parabolic dish antenna for the synthetic aperture radar (SAR) at one end. A 1-meter diameter parabolic dish antenna for the radio altimeter was also located at this end. The electrical axis of the radio altimeter antenna was lined up with the axis of the cylinder.

Most of the products are imported from China. Some products e.g. UPS, Stabilizers, dish-antenna and many type electronic kits are designed and assembled here. The products produced here are cheap but are of average or low quality.

This practice has raised some controversy within the industry, leading to the requirement that the satellite provider offer to install any extra dish antenna hardware for free and place a notice to this effect in place of any missing channels.

After the service interruption from Amos-4, DishHome managed to transmit its channels via Yamal 402 at 54.9°E, and requested customers to change the direction of their dish antenna to avail the service. On 19 July 2013, DishHome switched back its service through Amos-4 again.

Directivity is also defined for an antenna receiving electromagnetic waves, and its directivity when receiving is equal to its directivity when transmitting. The directivity of an actual antenna can vary from 1.76 dBi for a short dipole to as much as 50 dBi for a large dish antenna.

From April 16–18, 2010, again, the Arecibo Amateur Radio Club KP4AO conducted moon-bounce activity using the antenna. On November 10, 2013, the KP4AO Arecibo Amateur Radio Club conducted a Fifty-Year Commemoration Activation, lasting 7 hours on 14.250 MHz SSB, without using the main dish antenna.

The "Track 80" used an inflatable dish antenna to provide line-of-sight or tropospheric-scatter voice and teleprinter communications between missile firing units and higher headquarters. The erector-launcher, PTS, PS and RTS could be removed from the carriers and air-transported in fourteen CH-47 Chinook loads.

Type 984 3D radar on , 1961, using a Luneburg lens A Luneburg lens can be used as the basis of a high-gain radio antenna. This antenna is comparable to a dish antenna, but uses the lens rather than a parabolic reflector as the main focusing element. As with the dish antenna, a feed to the receiver or from the transmitter is placed at the focus, the feed typically consisting of a horn antenna. The phase centre of the feed horn must coincide with the point of focus, but since the phase centre is invariably somewhat inside the mouth of the horn, it cannot be brought right up against the surface of the lens.

In 1917, a fire tower (used for the visual location of forest fires) was constructed on Big Prospect. Beginning in 1951, the United States Air Force utilized Big Prospect for research purposes. They erected a large parabolic dish antenna in 1963. This necessitated relocation of the fire tower to Little Prospect.

The 18 m dish antenna installed at Fleurs in 1959 was transferred to the Parkes Observatory. Two of the old 13.7m dish antennas were relocated from the University of Sydney site to the CSIRO at Marsfield in 2005, as part of a precursor study into the Square Kilometer Array (SKA) development.

It was planned to feature a 9 m diameter dish antenna to observe in 8, 22 and 43 GHz bands, and was to be used in combination with ground radio telescopes to perform Very Long Baseline Interferometry. It was expected to achieve ten times higher resolution and ten times higher sensitivity than its predecessor HALCA.

Without RTSs, the SOCs would only be able to contact a satellite when it came into the control center's view. Some satellites, especially those in geostationary orbit, never come within view of their control center. Each antenna at an RTS is referred to as a "side". Previously, Side A typically included a dish antenna.

The SETI Institute named the telescope in Allen's honor. Overall, Paul Allen contributed more than $30 million to the project. The ATA is a centimeter-wave array which pioneers the Large-Number Small-Diameter concept of building radio telescopes. Compared to a large dish antenna, large numbers of smaller dishes are cheaper for the same collecting area.

The hovercraft carried a Decca 202 radar with a dish antenna, which could detect targets within . Some Army ACVs were fitted with XM3 Personnel Detectors (better known as XM-3 "people sniffers"), which could detect human emissions including carbon and ammonia. This equipment was used to find hidden enemies. Dog teams were also sometimes carried to help detect enemies.

A 2.6 m radio dish antenna for communications was also attached to the side of the cylinder. The spacecraft each massed 4000 kg. Both Venera 15 and 16 were equipped with a Synthetic Aperture Radar (SAR). A radar was necessary in this mission because nothing else would be able to penetrate the dense clouds of Venus.

The instrument is not an interferometer, but a phased array. A single dish antenna for these long wavelengths would have to be infeasibly large. Further, a phased array can be re-pointed at a different direction of observation instantaneously by changing the electronic signal delays between the individual antennas. The angular resolution is about 7° by 14°.

Uplink was via S band A two-axis steerable parabolic dish antenna with a diameter of approximately 1.5 m was attached at one edge of the orbiter base, and a fixed low-gain antenna extended from the top of the bus. Two tape recorders were each capable of storing 1280 megabits. A 381-MHz relay radio was also available.

Another was erected nearby for research towards the Ballistic Missile Early Warning System. The giant dish antenna stood as a local and marine navigational landmark until the current owners of the site, the Bevelaqua family, demolished it in 2007. In 1964 MIT sold the estate to the Society of Jesus of New England. It adapted the mansion as a religious retreat center.

While not yet confirmed, FM broadcast EME reception may also be possible using the Arecibo dish antenna. In 2002, physicist Dr. Tony Mann demonstrated that a single high-gain UHF yagi antenna, low noise masthead preamplifier, VHF/UHF synthesised communications receiver, and personal computer with FFT spectrum analyser software could be used to successfully detect extremely weak UHF television carriers via EME.

The original FPS-79 antenna at Diyarbakir had a unique feature which enhanced its Spacetrack usefulness. A variable-focus feed horn provided a wide beam for detection and a narrow beamwidth for tracking. That antenna was replaced by a new antenna and pedestal in 1975. Pulse compression was used to improve both the gain and resolution of the dish antenna.

The first astrometrical observation using all ten antennas was carried out on May 29, 1993. The total cost of building the VLBA was about $85 million. The array is funded by the National Science Foundation, and costs about $10 million a year to operate. Each receiver in the VLBA consists of a parabolic dish antenna 25 meters (82 feet) in diameter, along with its adjacent control building.

A despun dish antenna provided S and X band communication with Earth. A Star-24 solid rocket motor was integrated into the spacecraft to provide the thrust to enter orbit around Venus. From Venus orbit insertion to July 1980, periapsis was held between (at 17 degrees north latitude) to facilitate radar and ionospheric measurements. The spacecraft was in a 24-hour orbit with an apoapsis of .

For more demanding needs, some companies offer high-gain antennae for CubeSats, but their deployment and pointing systems are significantly more complex. For example, MIT and JPL are developing an inflatable dish antenna with a useful range to the Moon but appears to be poorly efficient. JPL has successfully developed X-band and Ka-band high-gain antennas for MarCO and Radar in a CubeSat (RaInCube) missions.

Ulysses spacecraft The spacecraft body was roughly a box, approximately 3.2 × 3.3 × 2.1 m (10.5 x 10.8 x 6.9 ft) in size. The box mounted the 1.65 m (5.4 ft) dish antenna and the GPHS-RTG radioisotope thermoelectric generator (RTG) power source. The box was divided into noisy and quiet sections. The noisy section abutted the RTG; the quiet section housed the instrument electronics.

The term "broadcast network" is often used to distinguish networks that broadcast an over-the-air television signals that can be received using a tuner (television) inside a television set with a television antenna from so-called networks that are broadcast only via cable television (cablecast) or satellite television that uses a dish antenna. The term "broadcast television" can refer to the television programs of such networks.

The spacecraft was of the Ranger Block I design and consisted of a hexagonal base across upon which was mounted a cone-shaped high tower of aluminum struts and braces. Two solar panel wings measuring from tip to tip extended from the base. A high-gain directional dish antenna was attached to the bottom of the base. Spacecraft experiments and other equipment were mounted on the base and tower.

Collins antenna design and development began in 1951 with the challenging design and construction of a 50-ft. diameter parabolic "dish" antenna for the Naval Research Laboratory in Washington DC. Collins antenna expertise expanded in the following years to include pioneering designs for satellites, deep space ground stations, HF ground communication, aircraft communication and navigation, spacecraft, commercial broadcast, microwave, and other special applications. Shanklin, J.R. 2010. Leading Antenna Engineer.

The 12.8m-wide Casshorn antenna, commissioned in October 1966, has interacting parabolic and hyperbolic reflectors in a characteristic "sugar scoop" form. It claims to be the only remaining example in the world. The larger 29.8m parabolic dish antenna was commissioned in late 1969. The OTC Satellite Earth Station Carnarvon, an Earth station in Australia, was established to meet the need for more reliable and higher quality communications for the Apollo program.

A large parabolic satellite communications antenna at Erdfunkstelle Raisting, the biggest facility for satellite communication in the world, in Raisting, Bavaria, Germany. It has a Cassegrain type feed. A parabolic antenna is an antenna that uses a parabolic reflector, 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.

Old (bottom) and new (top) Astro 60cm satellite dishes Astro broadcasts on Ku-band using the transponders of the MEASAT satellite system. The reception of the service signals uses a fixed 65-cm diameter dish antenna. Astro service is currently transmitting from 3 satellites, which are Measat 3, Measat 3a, and Measat 3b. Initially, the HDMI output of the B.yond PVR was disabled (including NJOI) if the user was not subscribed to the HD service.

Since the wavelengths being observed with these types of antennas are so long, the "reflector" surfaces can be constructed from coarse wire mesh such as chicken wire. At shorter wavelengths parabolic "dish" antennas predominate. The angular resolution of a dish antenna is determined by the ratio of the diameter of the dish to the wavelength of the radio waves being observed. This dictates the dish size a radio telescope needs for a useful resolution.

The Dominion Radio Astrophysical Observatory is a research facility founded in 1960 and located southwest of Okanagan Falls and Penticton. The site houses three instruments - an interferometric radio telescope, a single- dish antenna, and a solar flux monitor - and supports engineering laboratories. The DRAO is operated by the Herzberg Institute of Astrophysics of the National Research Council of the Canadian government. The observatory was named an IEEE Milestone for first radio astronomical observations using VLBI.

TESS spacecraft before launch In 2013, Orbital Sciences received a four-year, contract to build TESS for NASA. TESS uses an Orbital Sciences LEOStar-2 satellite bus, capable of three-axis stabilization using four hydrazine thrusters plus four reaction wheels providing better than three arc-second fine spacecraft pointing control. Power is provided by two single-axis solar arrays generating 400 watts. A Ka-band dish antenna provides a 100 Mbit/s science downlink.

In order to receive HRPT transmissions a high gain antenna is required, such as a small satellite dish, a helical antenna, or a crossed yagi. Basic reception equipment includes a parabolic dish antenna attached to an Azimuth-Elevation unit. The HRPT signal is further enhanced with a 1.7 GHz pre-amplifier. An HRPT receiver unit and a dish tracking controller are required to steer the Azimuth-Elevation unit controlling the parabolic dish.

The Haystack Observatory, run by MIT, developed a Small Radio Telescope (SRT) for educational purposes, consisting of a 2.3-meter diameter standard satellite dish antenna. This radio telescope operates at a 1.42 GHz frequency (21-cm wavelength) where hydrogen atoms emit a strong spectral line. This allows radio astronomers to detect hydrogen, the most abundant element of the Universe. One SRT has been donated to ISU by ESA and is operational since 2009.

Particularly "loud" components, such as the preamps for the radio dipole, were mounted outside the structure entirely, and the box acted as a Faraday cage. Ulysses was spin-stabilised about its z-axis which roughly coincides with the axis of the dish antenna. The RTG, whip antennas, and instrument boom were placed to stabilize this axis, with the spin rate nominally at 5 rpm. Inside the body was a hydrazine fuel tank.

Ranger 3. Ranger 3 was the first of the Block II Ranger designs. The basic vehicle was 3.1 m high and consisted of a lunar capsule covered with a balsa wood impact- limiter, 650 mm in diameter, a mono-propellant mid-course motor, a retrorocket with a thrust of 5080 pounds force (22.6 kN), and a gold- and chrome-plated hexagonal base 1.5 m in diameter. A large high-gain dish antenna was attached to the base.

It was instrumental in the development of TIROS-1 and TIROS-2 weather satellites. In 1953, the test site was sold by AT&T;, and the new owners leased the property to the U.S. Army Signal Corps for tracking satellites. A dish antenna on a tower (near the Bicentennial Oak Tree) was used to pick up signals from Russian satellites Sputnik 1 and Sputnik 2. The large circular concrete base of this antenna is still visible today.

Apollo 15 Lunar Module and Lunar Roving Vehicle, August 1, 1971. The S-band dish antenna for the rover is visible. The Unified S-band (USB) system is a tracking and communication system developed for the Apollo program by NASA and the Jet Propulsion Laboratory (JPL). It operated in the S band portion of the microwave spectrum, unifying voice communications, television, telemetry, command, tracking and ranging into a single system to save size and weight and simplify operations.

The system of gateways comprising the satellite ground system provides all network services for satellite and corresponding terrestrial connectivity. Each gateway provides a multiservice access network for subscriber terminal connections to the Internet. In the continental United States, because it is north of the equator, all gateway and subscriber dish antenna must have an unobstructed view of the southern sky. Because of the satellite's geostationary orbit, the gateway antenna can stay pointed at a fixed position.

The purpose of this experiment was to study the electromagnetic reflective properties of the lunar surface. The 136.10-MHz (2.2 m) telemetry transmissions from the spacecraft were scattered from the lunar surface and then recorded by use of the 150-ft Stanford dish antenna. The reflected signal intensity depended upon the lunar reflectivity, the spacecraft altitude above the lunar surface, and the mean curvature of the Moon. The returned signal bandwidth was proportional to RMS lunar surface slopes.

Mobile services, such as SiriusXM, and Worldspace, allow listeners to roam across an entire continent, listening to the same audio programming anywhere they go. Other services, such as Music Choice or Muzak's satellite-delivered content, require a fixed- location receiver and a dish antenna. In all cases, the antenna must have a clear view to the satellites. In areas where tall buildings, bridges, or even parking garages obscure the signal, repeaters can be placed to make the signal available to listeners.

A satellite truck is a mobile communications satellite earth station, typically mounted on a truck chassis as a platform. Employed in remote television broadcasts, satellite trucks transmit video signals back to studios or production facilities for editing and broadcast. Satellite trucks usually travel with a production truck, which contains video cameras, sound equipment and a crew. A satellite truck has a large satellite dish antenna which is pointed at a communications satellite, which then relays the signal back down to the studio.

These centers are equipped with C-band satellite dish antenna and high-speed broadband connection, these sites are able to receive real-time broadcast feeds emanating from the headquarters. Assigned church workers and officers oversee activities at locale chapters and receive queries regarding membership in the church. In 2012, a mobile coordinating center was launched including livelihood academy. A bus transformed into a cozy venue with roof, chairs, television screen and satellite receiver, can accommodate guests in remote areas during Bible Expositions.

The 20-meter dish antenna in Bochum Observatory, Germany, would be a support station. Although NASA was not funding the project, it made advisors available and gave approval to try to establish contact. On May 21, 2014, NASA announced that it had signed a Non- Reimbursable Space Act Agreement with the ISEE-3 Reboot Project. "This is the first time NASA has worked such an agreement for use of a spacecraft the agency is no longer using or ever planned to use again," officials said.

Its first dish, Antenna One (dubbed "Arthur"), was built in 1962 to link with Telstar. It was the first open parabolic design and is 25.9 metres (85 feet) in diameter and weighs 1,118 tonnes. After Pleumeur-Bodou Ground Station (Brittany) which received the first live transatlantic television broadcasts from the United States via the Telstar satellite at 0H47 GMT on 11 July 1962, Arthur received his first video in the middle of the same day. It is now a Grade II listed structure and is therefore protected.

The Dominion Radio Astrophysical Observatory is a research facility founded in 1960 and located at Kaleden, British Columbia, Canada. The site houses four radio telescopes: an interferometric radio telescope, a 26-m single-dish antenna, a solar flux monitor, and the Canadian Hydrogen Intensity Mapping Experiment (CHIME) — as well as support engineering laboratories. The DRAO is operated by the Herzberg Institute of Astrophysics of the National Research Council of the Government of Canada. The observatory was named an IEEE Milestone for first radio astronomical observations using VLBI.

Hope uses two 900-watt solar panels to charge its batteries, and it communicates with Earth using a high-gain -wide dish antenna. The spacecraft is equipped with star tracker sensors which help determine its position in space by identifying the constellations in relation to the Sun. Six 120-N thrusters control the speed of the probe, and eight 5-N reaction control system (RCS) thrusters are responsible for delicate maneuvers. The expected travel time of the Hope probe is about 200 days on its journey of .

Nozomi was to be inserted into a highly eccentric Mars orbit with a periareion 300 km above the surface, an apoareion of 15 Mars radii, and an inclination of 170 degrees with respect to the ecliptic plane. Shortly after insertion, the mast and antennas were to be deployed. The periareion would have been lowered to 150 km, the orbital period to about 38.5 hours. The spacecraft was to be spin stabilized at 7.5 rpm with its spin axis (and the dish antenna) pointed towards Earth.

They developed a program that simulated the effects of precession on the satellite's orbit, and used this information to calculate the percentage of time that sunlight fell on it. The result proved the system would have more than enough power. While it was designed with a lifetime of only one year, Alouette I eventually ran for ten years before being shut off. The computer was also put into use generating tracking commands for the receiver dish antenna in Ottawa that downloaded data from Alouette.

The system is reported to be of the frequency-agile monopulse type. It consists of an elliptical rotating surveillance antenna mounted on top of the array, operates in H band (6 to 8 GHz) and has a 30 km acquisition range against most targets. The large pulsed J band (14.5 GHz) engagement antenna is mounted below it in the centre of the array and has a maximum tracking range of about 20 km. Mounted on either side of the tracking radar antenna is a small J band parabolic dish antenna to track the missile.

After the end of the Soviet Union, two problems arose for the project. The first was geopolitical in nature: the main spacecraft control center was located at the Yevpatoria facility in the Crimea region. This control center was significant in the Soviet space program, being one of only two in the country equipped with a 70 m dish antenna. With the breakup of the Union, the Crimea region found itself part of the newly independent Ukraine and the center was put under Ukrainian national control, prompting new political hurdles.

Research-grade prototypes were developed with the hardware and software that were based on the OVSA system. The field testing started in 1994 with one antenna in Hawaii and the other antenna located near the OVSA site, about away from one of its antennas. SRBL was a spectrometer using an automated parabolic dish antenna with spiral antenna receiving element that was capable of observing 120 frequencies from 610 MHz to 18 GHz at 4.8 second interval. Additionally, 245 and 410 MHz frequencies can be observed from a dual Yagi antenna attached to the feed.

Internal view of a dome containing a dish antenna for satellite communications Svalbard Satellite Station () or SvalSat is a satellite ground station located on Platåberget near Longyearbyen in Svalbard, Norway. Opened in 1997, it is operated by Kongsberg Satellite Services (KSAT), a joint venture between Kongsberg Defence & Aerospace and the Norwegian Space Centre (NSC). SvalSat and KSAT's Troll Satellite Station (TrollSat) in Antarctica are the only ground stations that can see a low altitude polar orbiting satellite (e.g., in sun-synchronous orbit) on every revolution as the earth rotates.

SeaWinds used a rotating dish antenna with two spot beams that sweep in a circular pattern. The antenna consists of a 1-meter diameter rotating dish that produces two spot beams, sweeping in a circular pattern. It radiates 110 W microwave pulses at a pulse repetition frequency (PRF) of 189 Hz. QuikSCAT operates at a frequency of 13.4 GHz, which is in the Ku-band of microwave frequencies. At this frequency, the atmosphere is mostly transparent to non-precipitating clouds and aerosols, although rain produces significant alteration of the signal.

In January 2016, Sky Direct began the trial period for its prepaid service in three (3) areas through authorized dealers in Metro Manila, province of Cavite and Quezon. Sky Direct had a soft launching on March 18, 2016 by releasing the television commercial advertisement with endorser Kris Aquino. The Sky Direct prepaid subscription package includes a satellite dish antenna, set top box (Integrated Receiver-Decoder) and remote control. Sky Direct uses the DVB-S2 digital television broadcast standard in the Ku band to provide standard definition (SD) and high definition (HD) TV broadcasts.

Astro-G was selected in February 2006 against the competition of a proposed new X-Ray astronomy mission (NeXT) and a proposed solar sail mission to Jupiter. Funding started from FY 2007 with a budget of 12 billion yen, around 100 million US dollars. It was planned to be launched in 2012 but technical difficulty with the dish antenna as well as budget constraints led to putting development on hold for fiscal year 2010. Eventually the project was canceled in 2011 for the increased cost and the difficulty of achieving science goals.

G. Krishna Murthy), a small-time fish-selling agent, has deserted her and is living happily with his second wife Kunjipathu and their child Adda. A family gifts her a television with a satellite dish antenna in gratitude after she attends to a difficult delivery (for which they even had to bodily remove her from a movie theatre). The arrival of the first color TV in her small island village heralds great changes in the sleepy hamlet. The women in the village begin gathering at her house once the men leave for fishing.

The Northeastern Space Radio Observatory (Portuguese: Rádio-Observatório Espacial do Nordeste - ROEN) is a radio dish antenna located in the municipality of Eusébio in the state of Ceará, Brazil, approximately south of Fortaleza. The facility is owned by the National Institute for Space Research (INPE) and managed by the Center of Radio Astronomy and Astrophysics at Universidade Presbiteriana Mackenzie (CRAAM). It was initially funded by several by Brazilian institutions and the United States National Oceanic Atmospheric Administration (NOAA). It has been operating since 1993 and is used primarily for geodetic very long baseline interferometry (VLBI).

Each spacecraft was to carry solar panels that would be pointed toward the Sun and a dish antenna that would be pointed at Earth. Each would also carry a host of scientific instruments. Some of the instruments, such as cameras, would need to be point-ed at the target body it was studying. Other instruments were non-directional and studied phenomena such as magnetic fields and charged particles. JPL engineers proposed to make the Mariners “three-axis-stabilized,” meaning that unlike other space probes they would not spin.

Two solar panel wings, each 739 mm wide by 1537 mm long, extended from opposite edges of the base with a full span of 4.6 m, and a pointable high-gain dish antenna was hinge mounted at one of the corners of the base away from the solar panels. A cylindrical quasi-omnidirectional antenna was seated on top of the conical tower. The overall height of the spacecraft was 3.6 m. Propulsion for the mid-course trajectory correction was provided by a 224 N thrust monopropellant hydrazine engine with four jet-vane vector control.

Direct-to-home (DTH) service is a satellite broadcast service in which a large number of radio channels are digitally beamed down over a territory from a high-power satellite. AIR broadcasts various national and regional stations available to listen on DD Free Dish. The DTH signals can be received directly at homes using a small- sized dish receiver unit containing a dish antenna installed on a building’s rooftop or on a wall facing clear south and one indoors. DTH service is offered on twenty one channels via Insat.

The spacecraft used S-band for uplinked commands and downlinked telemetry, through dual redundant 5-watt transceivers. The spacecraft used X-band for science return (downlink only), using dual 20 W TWTAs until the failure of the last remaining TWTA in January 2008. Both bands used the dish antenna with prime-focus feeds, unlike the Cassegrain feeds of most other spacecraft dishes. Dual tape recorders, each of approximately 45-megabit capacity, stored science data between the nominal eight-hour communications sessions during the prime and extended mission phases.

The Nozomi orbiter was a 0.58 meter high, 1.6 meter square prism with truncated corners. Extending out from two opposite sides were solar panel wings containing silicon solar cells which provide power to the spacecraft directly or via NiMH (nickel metal hydride) batteries. On the top surface was a dish antenna, and a propulsion unit protrudes from the bottom. A 5 m deployable mast and a 1 m boom extended from the sides, along with two pairs of thin wire antennas which measure 50 m tip to tip.

The AN/FPS-17 Space Surveillance Radar developed by the Rome Air Development Center (RADC) was the first surveillance radar system designed to detect objects in space. The FPS-17 detection scanning radars have fixed antennae oriented toward the Soviet Union. The Air Force FPS-79 UHF tracking radar at Diyarbakir-Pirinçlik in Turkey is capable of tracking missiles during flight. The 10 meter diameter dish antenna system has a variable focus feed horn system which can provide a wide beam for target detection, and a narrow beam for tracking (other similar radars have scan rates in excess of {10^o} per second).

A high-gain directional dish antenna was attached to the bottom of the base. Spacecraft experiments and other equipment were mounted on the base and tower. Instruments aboard the spacecraft included a Lyman-alpha telescope, a rubidium-vapor magnetometer, electrostatic analyzers, medium-energy-range particle detectors, two triple coincidence telescopes, a cosmic-ray integrating ionization chamber, cosmic dust detectors, and scintillation counters. The communications system included the high-gain antenna and an omnidirectional medium-gain antenna and two transmitters at approximately 960 MHz, one with 0.25 W power output and the other with 3 W power output.

Ranger 5 was a Block II Ranger spacecraft similar to Ranger 3 and Ranger 4. The basic vehicle was 3.1 m high and consisted of a lunar capsule covered with a balsawood impact-limiter, 65 cm in diameter, a mono-propellant mid-course motor, a retrorocket with a thrust of 5080 lbf (23 kN), and a gold and chrome plated hexagonal base 1.5 m in diameter. A large high-gain dish antenna was attached to the base. Two wing-like solar panels (5.2 m across) were attached to the base and deployed early in the flight.

The satellites used for broadcasting television are usually in a geostationary orbit above the earth's equator. The advantage of this orbit is that the satellite's orbital period equals the rotation rate of the Earth, so the satellite appears at a fixed position in the sky. Thus the satellite dish antenna which receives the signal can be aimed permanently at the location of the satellite, and does not have to track a moving satellite. A few systems instead use a highly elliptical orbit with inclination of +/−63.4 degrees and orbital period of about twelve hours, known as a Molniya orbit.

The Tracking & Imaging Radar (TIRA) system serves as the central experimental facility for the development and investigation of radar techniques for the detection and reconnaissance of objects in space, and (to a certain degree) of air targets. TIRA has a 34-metre parabolic dish antenna is a monopulse radar operating at 1.333 GHz or 22.5 cm (L band) and 16.7 GHz or 1.8 cm (Ku band) wavelengths. The L-band is usually used for tracking debris with a 0.45° beam width, at 1 MW peak power. The system is capable of determining orbits from direction angles, range and Doppler shift for single targets.

It used the AS-1270/TRC-80 8 Foot Parabolic Antenna, an inflatable dish antenna that was stored in a recessed space in the roof of the shelter. The TRC-80 shelter was carried on an M474 tracked vehicle with Pershing 1; with Pershing 1a it was carried on the Ford M656 tractor by the U.S. Army and on a 5-ton Magirus-Deutz tractor by the German Air Force. With the introduction of Pershing II, the TRC-80 was replaced by the AN/TRC-184 Radio Terminal Set and the AN/MSC-6 Satellite Communication Terminal.

Ranger 6 in the Jet Propulsion Laboratory, Pasadena, California. Rangers 6, 7, 8, and 9 were called Block 3 versions of the Ranger spacecraft. The spacecraft consisted of a hexagonal aluminum frame base 1.5m across on which was mounted the propulsion and power units, topped by a truncated conical tower that held the TV cameras. Two solar panel wings, each 739mm wide by 1537mm long, extended from opposite edges of the base with a full span of 4.6m, and a pointable high-gain dish antenna was hinge mounted at one of the corners of the base away from the solar panels.

Millimeter Wave link installed in the UAE A point-to-point wireless unit with built-in antenna at Huntington Beach, California In modern computer networking, the term point-to- point telecommunications means a wireless data link between two fixed points. The telecommunications signal is typically bi-directional and either time division multiple access (TDMA) or channelized. This can be a microwave relay link consisting of a transmitter which transmits a narrow beam of microwaves with a parabolic dish antenna to a second parabolic dish at the receiver. It also includes technologies such as lasers which transmit data modulated on a light beam.

Radio astronomy became a prominent feature of post war astronomy in Canada with the construction of the Algonquin Radio Observatory in Algonquin Park, Ontario in 1959. This facility built under the direction of noted astronomer Dr. Arthur Covington, featured a large receiving dish. The Dominion Radio Astrophysical Observatory in Penticton, British Columbia, built shortly thereafter, features an interferometric radio telescope, a 26-m single-dish antenna and a solar flux monitor. In 1962 another optical telescope, a 48-inch reflector fitted with a Coude focus and a room sized spectrograph, was added to the Dominion Astrophysical Observatory in Victoria.

With the new VIII radar a uniform facility, Cunningham took over a Mosquito NF.XII—the first Mosquito to have a smooth "bluff" nose dome over the dish antenna. At this time the Luftwaffe was sending increased numbers of Focke-Wulf Fw 190 fighters over England, at night and at low-level. They were able to hit coastal targets and their speed and agility meant they were difficult to intercept. The German pilots were disadvantaged in some respects; there was a lack of night-flying experience in these units, the Fw 190s did not carry radar and had a short range.

The immense horn antenna within the radome at Andover Earth Station. This type of antenna is called a Hogg or horn-reflector antenna, invented by Albert Beck and Harald Friis in 1941 and further developed by D. L. Hogg at Bell Telephone Laboratories in 1961. It consists of a flaring metal horn with a metal reflector mounted in the mouth at a 45° angle. The advantage of this design over a parabolic dish antenna is that it has very low sidelobes; that is, the horn shields the antenna from radiation from angles outside the main beam axis, such as ground noise.

Dream Satellite TV was the first all-digital Direct-To-Home (DTH) television broadcasting service via satellite in the Philippines. Broadcasting from the Dream Broadcast Center located at the Clark Special Economic Zone in Pampanga. Content is received from program providers, compressed and broadcast via Koreasat 5 (Mugunghwa 5) in DVB-S and NTSC color format exclusively to its subscribers using the Integrated Receiver-Decoder and the Conax/Nagravision 3 Encryption System. To receive Dream's broadcasting signals, subscribers must acquire a in diameter satellite dish antenna, an Integrated Receiver-Decoder (IRD) and a Dream Conditional Access Card (Smart Card).

The frame was made of 2219 aluminium alloy tubing welded assemblies and consisted of a three-part chassis that was hinged in the center so it could be folded up and hung in the Lunar Module Quadrant 1 bay, which was kept open to space by omission of the outer skin panel. It had two side-by-side foldable seats made of tubular aluminium with nylon webbing and aluminum floor panels. An armrest was mounted between the seats, and each seat had adjustable footrests and a Velcro-fastened seat belt. A large mesh dish antenna was mounted on a mast on the front center of the rover.

Launch of Ranger 4 Ranger 4 was a Block II Ranger spacecraft virtually identical to Ranger 3. The basic vehicle was , high and consisted of a lunar capsule covered with a balsawood impact-limiter, in diameter, a mono-propellant mid-course motor, a thrust retrorocket, and a gold- and chrome-plated hexagonal base in diameter. A large high-gain dish antenna was attached to the base. Two wing-like solar panels ( across) were attached to the base and deployed early in the flight. Power was generated by 8,680 solar cells contained in the solar panels which charged an 1 kWh capacity AgZn launching and backup battery.

The higher frequency Ku-band systems tend to resemble DBS systems and can use a smaller dish antenna because of the higher power transmissions and greater antenna gain. TVRO systems tend to use larger rather than smaller satellite dish antennas, since it is more likely that the owner of a TVRO system would have a C-band-only setup rather than a Ku band-only setup. Additional receiver boxes allow for different types of digital satellite signal reception, such as DVB/MPEG-2 and 4DTV. The narrow beam width of a normal parabolic satellite antenna means it can only receive signals from a single satellite at a time.

GAGAN is now in operational phase and is compatible with other SBAS systems such as the wide-area augmentation system (WAAS), the European Geostationary Navigation Overlay Service (EGNOS) and the Multi-functional Satellite Augmentation System (MSAS) and will provide seamless air navigation service across regional boundaries. While the ground segment consists of eight reference stations and a master control center, which will have sub systems such as data communication network, SBAS correction and verification system, operations and maintenance system, performance monitoring display and payload simulator, Indian land uplinking stations will have dish antenna assembly. The space segment will consist of one geo-navigation transponder.

Artist impression of Ranger 9's last seconds. Rangers 6, 7, 8, and 9 were the so-called Block 3 versions of the Ranger spacecraft. The spacecraft consisted of a hexagonal aluminium frame base 1.5 m across on which was mounted the propulsion and power units, topped by a truncated conical tower which held the TV cameras. Two solar panel wings, each 739 mm wide by 1537 mm long, extended from opposite edges of the base with a full span of 4.6 m, and a pointable high-gain dish antenna was hinge mounted at one of the corners of the base away from the solar panels.

Launch of Atlas Agena B with Ranger 7. Rangers 6, 7, 8, and 9 were called Block 3 versions of the Ranger spacecraft. The spacecraft consisted of a hexagonal aluminum frame base 1.5 m across on which was mounted the propulsion and power units, topped by a truncated conical tower which held the TV cameras. Two solar panel wings, each 739 mm wide by 1537 mm long, extended from opposite edges of the base with a full span of 4.6 m, and a pointable high-gain dish antenna was hinge mounted at one of the corners of the base away from the solar panels.

The 'Kennedy Dish' antenna was transferred from the Fleurs Observatory (where it was part of the Chris Cross Telescope) in 1963. Mounted on rails and powered by a tractor engine to allow the distance between the antenna and the main dish to be easily varied, it was used as an interferometer with the main dish. Phase instability due to an exposed cable meant that its pointing ability was diminished, but it was able to be used for identifying size and brightness distributions. In 1968 it successfully proved that Radio galaxy lobes were not expanding, and in the same era contributed to Hydrogen line and OH investigations.

He joined the Indian Space Research Organisation (ISRO) and started his career at its ISRO Telemetry, Tracking and Command Network (ISTRAC), Sriharikota in 1976. He later worked in its Indian Space Research Organisation Satellite Centre (ISAC) from 1978 to 1998. He was the project director for the development of the dish antenna of the Indian Deep Space Network which is used for telemetry for the missions such as the Chandrayaan-1, India's first lunar exploration mission and Mangalyaan, India's first interplanetary mission. He was involved in several satellite missions such as Bhaskara, Indian National Satellite System (INSAT), Ariane Passenger Payload Experiment (APPLE) and Indian Remote Sensing Programme (IRS).

In its area of influence two Argentine-built refuges existed since long before: the Sargento Ayudante Cisterna y el Aviso ARA Comandante Zapiola shelters had been set up in January 1976. In addition to new instruments brought from the mainland, Belgrano II received all the scientific equipment transferred from Belgrano I. The LABEL laboratory (LAboratory BELgrano) was rebuilt demanding considerable effort. A new facility, the José Luis Sersic polar astronomical observatory and a satellite dish antenna for data transmission were also set up. On the morning of 10 September 2005 the main house was completely destroyed as a result of a fire caused by a heater malfunction.

Operations are supported by donations from loyal viewers. In 2009, a severe thunderstorm late on the evening of July 11 seriously damaged the new radio tower at its new TV studio, which holds the microwave-band dish antenna for the studio/transmitter link. In use for less than two weeks, it was made necessary because of a move in the studio location further away from the TV transmitter site, making the cost of leasing a much longer fiber-optic line than before prohibitive. K38HE went off the air couple of times after a transmitter tube broke in the transmitter and returned to the air on October 9, 2009.

Communications consisted of a 3-watt transmitter capable of continuous telemetry operation, the large high gain directional dish antenna, a cylindrical omnidirectional antenna at the top of the instrument mast, and two command antennas, one on the end of either solar panel, which received instructions for midcourse maneuvers and other functions. Propulsion for midcourse maneuvers was supplied by a monopropellant (anhydrous hydrazine) 225 N retro-rocket. The hydrazine was ignited using nitrogen tetroxide and aluminum oxide pellets, and thrust direction was controlled by four jet vanes situated below the thrust chamber. Attitude control with a 1 degree pointing error was maintained by a system of nitrogen gas jets.

Attached by an arm to one side of the base and extending below the spacecraft was a large directional dish antenna. The Mariner 1 power system consisted of the two solar-cell wings, one , and the other , with a dacron extension (a solar sail) to balance the solar pressure on the panels. Those panels powered the craft directly or recharged a 1000-watt-hour sealed silver–zinc cell battery, which was to be used before the panels were deployed, when the panels were not illuminated by the Sun, and when loads were heavy. A power-switching and booster regulator device controlled the power flow.

Communications consisted of a 3-watt transmitter capable of continuous telemetry operation, the large high-gain directional dish antenna, a cylindrical omnidirectional antenna at the top of the instrument mast, and two command antennas, one on the end of either solar panel, which received instructions for midcourse maneuvers and other functions. Propulsion for midcourse maneuvers was supplied by a monopropellant (anhydrous hydrazine) 225 N retro-rocket. The hydrazine was ignited using nitrogen tetroxide and aluminium oxide pellets, and thrust direction was controlled by four jet vanes situated below the thrust chamber. Attitude control with a 1° pointing error was maintained by a system of nitrogen gas jets.

Alvarion WiMAX Customer-premises equipment Alvarion Technologies provides Wi-Fi solutions for Smart Cities, mobile carriers, enterprises, smart hospitality, campuses and High-Density Events. It was one of the first companies to produce IEEE 802.11 wireless LAN equipment and made some contributions to the development of the IEEE 802.11 standard. In collaboration with the Swedish Space Corporation and using its own BreezeNET DS.11 product, it also claims to hold a World record of longest Wireless LAN link ever achieved – from ground to a weather balloon (although it had been heavily amplified, used a huge dish antenna, and had an automatic tracking system). This record is not found in The Guinness Book of Records, however.

The ventral hemispherical radome for the H2X's rotating dish antenna replaced the ball turret on B-17 Flying Fortress Pathfinders, with the electronics cabinets for the "Mickey set" being installed in the radio room just aft of the bomb bay. The H2X on later B-24 Liberators also replaced the ball turret, being made retractable as the ball turret was for landing on the Liberator. The operators panel was installed on the flight deck behind the co-pilot (where the radio operator's normal position was). In combat areas the Mickey operator directed the pilot on headings to be taken, and on the bomb run directed the airplane in coordination with the bombardier.

In 1990, Air Force Space Command established a tenant unit at San Vito Air Station. Detachment 1, 73rd Space Surveillance Group was a deep space surveillance mission whose job was to search for earth- orbiting objects, generate positional (Element Set) data to identify the objects location in space, and provide that data to the Cheyenne Mountain Space Surveillance Center located in Cheyenne Mountain, Colorado Springs, Colorado. The detachment consisted of a Transportable Optical System (TOS) and a large signal detection dish antenna. The TOS, developed by Sandia National Laboratories, was a high resolution telescope used to detect visible light reflected off orbiting objects, while the large receiver dish passively received transmission signals from orbiting satellites.

In common with Explorer 6, Pioneer 5 used the earliest known digital telemetry system used on spacecraft, codenamed "Telebit", which was a tenfold (or 10 dB) improvement in channel efficiency on previous generation "Microlock" analog systems in use since Explorer 1 and the biggest single improvement in signal encoding on western spacecraft. The spacecraft received the uplink carrier at 401.8 MHz and converted it to a 378.2 MHz signal using a 16/17 coherent oscillator circuit. The telemetry system phase modulated a 512 Hz subcarrier, which was in turn amplitude modulated at 64, 8, or 1bit/s. The spacecraft was unable to aim its antennas, and so had no high-gain dish antenna common on later spacecraft.

Form of classic parabolic dish antenna and parabolic torus reflector antenna Simulsat antenna in Miami with casing for several LNBs A parabolic torus reflector antenna is a quasi-parabolic antenna, where the defining parabola is not rotated around the main transmission axis, but around an axis which stands vertically to this axis. Simulsat is a trademark for such antennas designed and manufactured by Antenna Technology Communications. Whereas parabolic satellite dishes with one low-noise block converter (LNB) are able to receive a satellite television broadcast from one communications satellite at a time, parabolic torus reflector antennas are capable of establishing views to more than 40 C and Ku band satellites simultaneously, by employing multiple LNBs.

Solar parabolic dish With a parabolic dish collector, one or more parabolic dishes concentrate solar energy at a single focal point, similar to the way a reflecting telescope focuses starlight, or a dish antenna focuses radio waves. This geometry may be used in solar furnaces and solar power plants. The shape of a parabola means that incoming light rays which are parallel to the dish's axis will be reflected toward the focus, no matter where on the dish they arrive. Light from the sun arrives at the Earth's surface almost completely parallel, and the dish is aligned with its axis pointing at the sun, allowing almost all incoming radiation to be reflected towards the focal point of the dish.

Attached by an arm to one side of the base and extending below the spacecraft was a large directional dish antenna. The power system of Mariner 2 consisted of two solar cell wings, one 183 cm by 76 cm and the other 152 cm by 76 cm (with a 31 cm dacron extension (a solar sail) to balance the solar pressure on the panels), which powered the craft directly or recharged a 1000 watt-hour sealed silver-zinc cell battery. This battery was used before the panels were deployed, when the panels were not illuminated by the Sun, and when loads were heavy. A power-switching and booster regulator device controlled the power flow.

Toruń 32-metre antenna – RT4 Toruń 15-metre antenna – RT3 The Institute of Astronomy of Nicolaus Copernicus University in Toruń, known prior to 1 October 2019 in scientific publications as the Toruń Centre for Astronomy, is an optical and radio observatory located at () in Piwnice, about 15 km north of Toruń, Poland. It houses two single-dish antenna telescopes, 32 metres and 15 metres in diameter, as well as the largest Polish optical telescope – 90 cm Schmidt-Cassegrain camera. The facility is operated by the Nicolaus Copernicus University. Also, photometry using 60 cm Cassegrain telescope is made and radio measurements of the Sun at 127 MHz frequency have been recorded on a daily basis since 1958 using a 23 m interferometer.

Attitudes changed in late 1938, when a full development contract was received from the Luftwaffe. The resulting system, known as the FuMG 62, as well as the prototype system FuMG 39T Darmstadt were demonstrated to Hitler at Rechlin in July 1939. The Telefunken team developed an accurate system based on a klystron microwave tube operating in the range of —an extremely short wavelength for the time—with a pulse length of 2 microseconds, a peak power of and a pulse repetition frequency (PRF) of 3,750 Hz. It had a maximum range of about and was accurate to about in range. Würzburg used a paraboloid dish antenna, which could be "folded" along the horizontal midline for travel on a wheeled trailer.

Earlier in 2014, officials with the Goddard Space Flight Center said the Deep Space Network equipment necessary to transmit signals to the spacecraft had been decommissioned in 1999, and was too expensive to replace. However, project members were able to find documentation for the original equipment and were able to simulate the complex modulator/demodulator electronics using modern software-defined radio (SDR) techniques and open-source programs from the GNU Radio project. They obtained the needed hardware, an off-the-shelf SDR transceiver and power amplifier, and installed it on the 305-meter Arecibo dish antenna on May 19, 2014. Once they gained control of the spacecraft, the capture team planned to shift the primary ground station to the 21-meter dish located at Kentucky's Morehead State University Space Science Center.

The spacecraft was an octagonal prism 1.88 m high and 1.14 m across with two solar panels protruding on opposite sides parallel to the axis of the prism. A high-gain fixed dish antenna was at one end of the prism, and the 489 N thruster at the other end. The sensor openings were all located together on one of the eight panels, 90 degrees from the solar panels, and protected by a single sensor cover. The spacecraft propulsion system consisted of a monopropellant hydrazine system for attitude control and a bipropellant nitrogen tetroxide and monomethyl hydrazine system for the maneuvers in space. The bipropellant system had a total Delta-v capability of about 1,900 m/s with about 550 m/s required for lunar insertion and 540 m/s for lunar departure.

A simpler two-position remote switch operated by a 22 kHz tone is also occasionally used for North American reception, but this configuration is not compatible with European- style universal LNB's which use the tone internally for band-switching. A toroidal antenna may be used with multiple LNB's to receive multiple satellites in various locations over a 40° arc. Unlike the single parabola of a standard satellite dish antenna (which is best adapted to focus one target satellite to a single point), the toroidal antenna uses a reflector pair to focus multiple signals to a line. Individual adjacent or near-adjacent pairs (such as Glorystar on 97°W and 101°W) may be received, due to their close proximity, with two LNB's on what otherwise looks geometrically to be a standard parabolic dish.

In the 1970s, Leighton's interest shifted to the development of large, inexpensive dish antenna which could be used to pursue millimeter-wave interferometry and submillimeter-wave astronomy. Once again, his remarkable experimental abilities opened a new field of science at Caltech which continues to be vigorously pursued at the Owens Valley Radio Observatory in California and the Caltech Submillimeter Observatory on Mauna Kea, Hawaii using the "Leighton Dishes". Leighton was an elected member of the National Academy of Sciences and served on its Space Science Board. Leighton shared the Rumford Prize in 1986 for advancements in Infrared Astronomy, and won the James Craig Watson Medal in 1988, for his work as creator and exploiter of new instruments and techniques that opened whole new areas of astronomy — solar oscillations, infrared surveys, spun telescopes, and large millimeter-wave reflectors.

Satellite Internet generally relies on three primary components: a satellite, typically in geostationary orbit (sometimes referred to as a geosynchronous Earth orbit, or GEO), a number of ground stations known as gateways that relay Internet data to and from the satellite via radio waves (microwave), and a small antenna at the subscriber's location, often a VSAT (very-small-aperture terminal) dish antenna with a transceiver. Other components of a satellite Internet system include a modem at the user end which links the user's network with the transceiver, and a centralized network operations center (NOC) for monitoring the entire system. Working in concert with a broadband gateway, the satellite operates a Star network topology where all network communication passes through the network's hub processor, which is at the center of the star. With this configuration, the number of remote VSATs that can be connected to the hub is virtually limitless.

While the rotating dish antenna can no longer spin as designed, the rest of the instrument remains functional and data transmission capabilities remain intact, although it cannot determine the surface vector wind. It can, however, still measure radar backscatter at a fixed azimuth angle. QuikSCAT is being used in this reduced mode to cross-calibrate other scatterometers in hopes of providing long-term and consistent surface wind datasets over multiple on-orbit scatterometer platforms, including the operational European Organisation for the Exploitation of Meteorological Satellites (EUMETSAT) Advanced Scatterometer (ASCAT) on MetOp-A and MetOp-B, India's Oceansat-2 scatterometer operated by the Indian Space Research Organization (ISRO), and the China's HaiYang-2A (HY-2A) scatterometer operated by China's National Satellite Ocean Application Service, as well as future NASA scatterometer missions in development. A NASA Senior Review panel in 2011 endorsed the continuation of the QuikSCAT mission with these modified objectives through 2018.

The free-to-view system contrasts with free-to-air (FTA), in which signals are transmitted in the clear, without encryption, and can be received by anyone with a suitable receiving dish antenna and DVB-compliant receiver (although these services can include proprietary encrypted data services such as an EPG that is only available to reception equipment made for, or authorised by, the FTA broadcaster). Free-to- view services are broadcast encrypted and can only be viewed with reception equipment that includes a suitable conditional-access module and viewing card, in the same way as a pay-TV satellite service. However, the FTV service viewing card is not subject to a continuing subscription payment for viewing the service's channels and may be available for a regular fee, a one-off payment or even for free. Services which charge a regular fee for reception can still be considered free-to-view, and not pay-TV if the fee is not for the programming content but for the delivery.

WRMW "Radio Maria" (for: Radio Maria-Wisconsin) is a non-commercial FM broadcasting station at 91.3 MHz licensed to Peshtigo, Wisconsin serving the Sturgeon Bay area with Catholic programming. WRMW's signal and tower height also has the potential to reach into portions of the southern tip of the Upper Peninsula of Michigan and the western coast of the Lower Peninsula of Michigan. WRMW began as a construction permit licensed in May 2007 to its founder "Friends of Radio Maria" (which also airs Italian language Catholic programming on the FM subcarrier of New York station WKTU and on the internet.) WRMW is now owned and operated (and licensed to) Radio Maria Inc. Upon its initial sign-on which took place on May 26, 2010 just days before the construction permit expiration date, WRMW initially aired separate pre- recorded programming from the network archives while it was awaiting the installation of its satellite receiver and dish antenna from originating station KJMJ 580 kHz in Alexandria, Louisiana.

Night fighter, new fuselage with A-series' ventral Bola (Bodenlafette) gondola omitted, tail section from Ju 188, aerodynamically improved conformal gun pod for a quartet of forward-firing calibre, MG 151/20 autocannons below the former bomb bay. ;Ju 88 G-1 :BMW 801 radial engines with , FuG 220 Lichtenstein SN-2 radar ;Ju 88 G-6 :Junkers Jumo 213A inverted V12 engines with , used either FuG 220 Lichtenstein SN-2 90 MHz or FuG 218 Neptun 158/187 MHz frequency radar, either with the usual Hirschgeweih eight-dipole aerial setup or experimentally with the more aerodynamic Morgernstern tripled crossed-dipole aerials. Some very-late-war aircraft equipped with experimental FuG 240 Berlin cavity magnetron based 3 GHz radar, with dish antenna in bulbous solid nose. Optional with Schräge Musik upward firing guns with two guns. ;Ju 88 G-7 :Identical to G-6, but with Jumo 213E high-altitude engines, planned for use with FuG 218/220 with Morgenstern array or FuG 240.

This gap has been known as Baade's Window ever since. At Dover Heights in Sydney, Australia, a team of radio astronomers from the Division of Radiophysics at the CSIRO, led by Joseph Lade Pawsey, used 'sea interferometry' to discover some of the first interstellar and intergalactic radio sources, including Taurus A, Virgo A and Centaurus A. By 1954 they had built an fixed dish antenna and used it to make a detailed study of an extended, extremely powerful belt of radio emission that was detected in Sagittarius. They named an intense point-source near the center of this belt Sagittarius A, and realised that it was located at the very center of our Galaxy, despite being some 32 degrees south-west of the conjectured galactic center of the time. In 1958 the International Astronomical Union (IAU) decided to adopt the position of Sagittarius A as the true zero co- ordinate point for the system of galactic latitude and longitude.

A dish antenna at Stanford University was used to monitor Soviet radar signals after they bounced off the Moon. Chinese missile and nuclear programs were also monitored; for much of this the U-2 spy-plane was employed, including the ability to determine operating facilities by measuring their heat using infrared cameras, and to collect high-altitude gas samples from nuclear facility emissions.Opt. Cet, Richelson, pp. 93-96 CORONA missions also continued, primarily using the KH-4A (1963–1964) and KH-4B (1967) satellites. These had resolutions of about and , respectively, and carried two reentry vehicles, allowing each mission to cover some 18 million square miles.Opt. Cet., Richelson, p, 122 While the activities of Duckett and the FMSAC were of great value to the CIA, they mainly involved analyses of existing events. Some of the Agency’s strategic consultants strongly suggested that more capability was needed in advancing the basic science and technology used both in collecting information and in predicting future actions of adversaries. This would involve increasing the size and capabilities of not just the FMSAC but those of Wheelon’s overall organization.

The radio telescope at Parkes (Parkes Observatory), New South Wales, was used by NASA throughout the Apollo program to receive signals in the Southern Hemisphere, along with the NASA Honeysuckle Creek Tracking Station near Canberra. In the days before the July 1969 space mission that marked humanity's first steps on the Moon, NASA was working with a group of Australian technicians who had agreed to engineer a space-to-Earth interface to carry the video and telemetry signals from the Lunar Lander Eagle on the Moon and relay them to the rest of the global audience, estimated then at some 600 million people. The dish antenna used had to be large, as the signals expected from the spacecraft were very weak and easily lost; NASA had to use the Parkes radio telescope, situated in the middle of an Australian sheep farm. There were some background concerns at NASA about using the Parkes antenna, mainly technical, as the signals had to go via point-to-point microwave links to get re-transmitted globally.