Interferometers Interferometers The 4C Array is a cylindrical paraboloid radio telescope at the Mullard Radio Astronomy Observatory, similar in design to the Molonglo Observatory Synthesis Telescope. It is 450 m long, 20 m wide, with a second, moveable element (now mostly removed; some of it is still visible, beyond COAST). The first large aperture synthesis telescope ( 1958), it was also the first new instrument to be built at Lord's Bridge, after the Observatory was moved there in 1957, and needed 64 km (40 miles) of reflector wire (since removed). The 4C operated at 178 MHz (1.7 m), and located nearly 5000 sources of the 4C (4th Cambridge) catalogue published in 1965 and 1966, which helped establish the evolution of the radio galaxy population of the universe. The telescope is now inoperable. ...more on Wikipedia about "4C Array"
The Arcminute Microkelvin Imager (AMI) is an interferometer radio telescope designed principally to image secondary anisotropies in the cosmic microwave background (CMB) at higher angular resolution than the Very Small Array. It consists of two interferometric arrays sited at the Mullard Radio Astronomy Observatory in Cambridge, both operating in the frequency range 12-18 GHz. The short baseline array consists of ten 3.7-m parabolic antennae while the long-baseline array is composed of seven 13m antennae. ...more on Wikipedia about "Arcminute Microkelvin Imager"
The Australia Telescope Compact Array is a radio telescope at the Paul Wild Observatory, twenty five kilometres west of the town of Narrabri in Australia. ...more on Wikipedia about "Australia Telescope Compact Array"
The Caltech Submillimeter Observatory (or CSO) is a 10.4 m (34 ft) diameter submillimeter wavelength telescope situated alongside the 15 m James Clerk Maxwell submillimeter telescope (JCMT) at Mauna Kea Observatory. ...more on Wikipedia about "Caltech Submillimeter Observatory"
The Cambridge Interferometer was a radio telescope interferometer built by Martin Ryle and Antony Hewish in the early 1950s to the west of Cambridge (between the Grange Road football ground and the current Cavendish Laboratory). The interferometer consisted of an array of 4 fixed elements to survey the sky, and produced the 2C catalogue of radio sources at 81.5 MHz, and the 3C catalogue of radio sources at 159 MHz discovering some of the most interesting astronomical objects known. The telescope was operated by the Radio Astronomy Group of Cambridge University. ...more on Wikipedia about "Cambridge Interferometer"
The Cambridge Low-Frequency Synthesis Telescope (CLFST) is an east-west aperture synthesis radio telescope currently operating at 151 MHz. It consists of 60 tracking yagis on a 4.6 km baseline, giving 776 simultaneous baselines. These provide a resolution of 70×70 cosec(declination) arcsec2, with a sensitivity of about 30 to 50 mJy/beam, and a field of view of about 9°×9°. The telescope is situated at the Mullard Radio Astronomy Observatory. ...more on Wikipedia about "Cambridge Low Frequency Synthesis Telescope"
COAST, the Cambridge Optical Aperture Synthesis Telescope, is a multi-element optical interferometer with baselines of up to 100 metres, designed to observe stars with angular resolution as high as one thousandth of one arcsecond (producing images with much higher resolution than can be obtained using individual telescopes such as the Hubble Space Telescope). The principal limitation is that COAST can only image bright stars. COAST was the first long-baseline interferometer to obtain high-resolution images of the surfaces of stars other than our sun (although the surfaces of other stars had previously been imaged using Aperture Masking Interferometry on the William Herschel Telescope). ...more on Wikipedia about "Cambridge Optical Aperture Synthesis Telescope"
The CHARA Array is an astronomical optical interferometer operated by The Center for High Angular Resolution Astronomy (CHARA) at Georgia State University. CHARA is the World's highest angular resolution telescope at infrared wavelengths. The array will eventually have six 1-metre diameter telescopes, making it one of the most powerful imaging interferometers in the world. ...more on Wikipedia about "CHARA array"
The Cosmic Anisotropy Telescope CAT was a three-element interferometer for cosmic microwave background observations at 13 to 17 GHz, based at the Mullard Radio Astronomy Observatory. It was the first instrument to measure small-scale structure in the cosmic microwave background radiation in 1995. When the more sensitive Very Small Array came online, the CAT telescope was decomissioned in a ceremonial bonfire. ...more on Wikipedia about "Cosmic Anisotropy Telescope"
Darwin is a proposed European Space Agency (ESA) mission designed to directly detect Earth-like planets orbiting nearby stars, and search for evidence of life on these planets. The launch date will be at or after 2014. The current design envisions six telescopes, each 1.5 meters diameter, flying in formation. In addition, two auxiliary spacecraft would be needed, one to combine the light from the six telescopes and measure the resulting optical signal, and one to handle communications with Earth. As well as studying extrasolar planets, the instrument will probably have a general purpose imaging mode which will produce very high resolution (i.e. milliarcsecond) infrared images, allowing detailed study of a variety of astrophysical processes. ...more on Wikipedia about "Darwin (ESA)"
(Electron interferometer) ==Overview== ...more on Wikipedia about "Electron interferometer"
The European VLBI Network (EVN) was formed in 1980 by a consortium of five of the major radio astronomy institutes in Europe (the European Consortium for VLBI). Since 1980, the EVN and the Consortium has grown to include 9 institutes with 12 radio telescopes in 8 western European countries as well as associated institutes with telescopes in Poland, Russia, Ukraine and China. Proposals for additional telescopes in Spain and Italy are under consideration, and furthermore, the EVN can be linked to the 7-element Jodrell Bank MERLIN interferometer in the UK and to the US Very Long Baseline Array (VLBA) to create a " global network" . In 1993 the Joint Institute for VLBI in Europe ( JIVE) was created, with the Netherlands Foundation for Research in Astronomy (Dwingeloo) acting as the host institute. It will provide both scientific user support and a correlator facility. Very Long Baseline Interferometry (VLBI) achieves ultra-high angular resolution and is a multi-disciplinary technique e.g. imaging of extragalactic radio sources, geodesy and astrometry. ...more on Wikipedia about "European VLBI Network"
(Fabry-Perot interferometer) :Etalon redirects here. étalon is also the French word for stallion. ...more on Wikipedia about "Fabry-Perot interferometer"
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Giant Metrewave Radio Telescope (GMRT), located near Pune in India, is the world's largest radio telescope at metre wavelengths. It is operated by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research, Bombay. An office of NCRA is located in the Pune University campus right next to IUCAA. There are fourteen telescopes randomly arranged in the central square, with a further sixteen arranged in three arms of a "Y"-shaped array (similar to the VLA) giving an interferometric baseline of about 25 km. The GMRT is an interferometer which uses a technique known as aperture_synthesis to make images of radio sources. ...more on Wikipedia about "Giant Metrewave Radio Telescope"
In optics, a Gires-Tournois etalon is a transparent plate with two reflecting surfaces, one of which has very high reflectivity. Due to multiple-beam interference, light incident on the lower-reflectivity surface of a Gires-Tournois etalon is (almost) completely reflected, but has a phase shift that depends strongly on the wavelength of the light. ...more on Wikipedia about "Gires-Tournois etalon"
The Grand Interferometre a 2 Telescopes is an Optical Interferometer, on Plateau du Calern, Departement Fresnel, Observatoire de la Côte d'Azur, France. ...more on Wikipedia about "Grand Interferometre a 2 Telescopes"
The HALCA (Highly Advanced Laboratory for Communications and Astronomy) satellite is an 8 meter diameter radio telescope used for Very Long Baseline Interferometry. It is now in an orbit with an apogee altitude of 21,400 km and a perigee altitude of 560 km. The elliptical orbit will allow imaging of celestial radio sources by the satellite and ground based telescopes, with good (u,v) plane coverage and high resolution. The orbit has an inclination of 31 degrees, and a period of about 6.3 hours. It was launched in February 1997. After three years of designed life, altitude control failed in 2003, and the operation officially ended in November 2005. ...more on Wikipedia about "HALCA"
The Half-Mile Telescope was constructed in 1968 (2 aerials) at the Mullard Radio Astronomy Observatory with 2 more aerials being added in 1972, using donated dishes (total cost was £70,000). Two of the dishes are fixed, while two are moveable and share the One-Mile's rail track; to obtain information from the maximum number of different baselines, 30 days of observing were required. Observing frequency 1.4 GHz (21 cm wavelength), bandwidth 4 MHz. Used for Hydrogen Line studies of nearby galaxies and produced the first good radio maps of hydrogen distribution (as a function of its velocity), for M33 and M31 (also produced nearly 20 PhDs and 50 published papers). The telescope was operated by the Radio Astronomy Group of the Cambridge University. ...more on Wikipedia about "Half-Mile Telescope"
The Infrared Optical Telescope Array (IOTA) began with an agreement in 1988 among five Institutions, the Smithsonian Astrophysical Observatory, Harvard University, the University of Massachusetts, the University of Wyoming, and MIT/ Lincoln Laboratory, to build a two-telescope stellar interferometer for the purpose of making fundamental astrophysical observations, and also as a prototype instrument on which we could perfect techniques which could later lead to the development of a larger, more powerful array. On site construction went on for all 1993 and 1994, with first fringes in December 1993. ...more on Wikipedia about "Infrared Optical Telescope Array"
An intensity interferometer is the name given to devices that use the Hanbury-Brown and Twiss effect. In astronomy, the most common use of such an interferometer is to determine the apparent angular diameter of a radio source or star. If the distance to the object can then be determined by parallax or some other method, the physical diameter of the star can then be inferred. An example of an optical intensity interferometer is the Narrabri Stellar Intensity Interferometer. In quantum optics, some devices which take advantage of correlation and anti-correlation effects in beams of photons might be said to be intensity interferometers, although the term is usually reserved for observatories. ...more on Wikipedia about "Intensity interferometer"
The interferometric visibility (also known as "interference visibility" or just "visibility") quantifies the contrast of interference in any system which has wave-like properties, such as optics, quantum mechanics, water waves, or electrical signals. Generally, two or more waves are combined and as the phase between them is changed (e.g. in an interferometer) the power or intensity (or population in quantum mechanics) of the resulting wave oscillates (forming an interference pattern). The ratio of the size or amplitude of these oscillations to the sum of the powers of the individual waves is defined as the visibility. ...more on Wikipedia about "Interferometric visibility"
Interferometry is the applied science of combining two or more input points of a particular data type, such as optical measurements, to form a greater picture based on the combination of the two sources. In astronomy (such as with the Keck telescopes), this is used to combine light from two or more telescopes to obtain measurements with higher resolution than could be obtained with either telescope individually. ...more on Wikipedia about "Interferometry"
The James Clerk Maxwell Telescope (JCMT) is a 15-metre submillimetre-wavelength telescope at Mauna Kea Observatory in Hawaii. It is the largest astronomical telescope in the world designed specifically to operate in the submillimetre regime (between the far-infrared and the microwave regions of the electromagnetic spectrum). It is used to study our Solar System, interstellar dust and gas, and distant galaxies. ...more on Wikipedia about "James Clerk Maxwell Telescope"
The Keck Interferometer is part of NASA's overall effort to find planets and ultimately life beyond our solar system. It will combine the light from the twin Keck telescopes to measure the emission from dust orbiting nearby stars, directly detect the hottest gas giant planets, image disks around young stars and other objects of astrophysical interest, and survey hundreds of stars for the presence of planets the size of Uranus or larger. ...more on Wikipedia about "Keck Interferometer"
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