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Topic: Cambridge Interferometer

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	Scientific American: What is an optical interferometer, such as the one being developed at Palomar Mountain? ...
		Interferometers are now widely used for spectroscopy, the study of thin films, the testing of precision optics, measurements of refractive indices, and both radio and optical astronomy.
		The fringes are a striking example of the wave nature of light: the wavefronts add constructively or destructively, depending on the path difference between the wavefronts, and produce fringes that appear as bright and dark bands, with the bright bands being brighter than the sum of intensities in the two separate wavefronts.
		"Interferometers are used as a tool for stellar astrophysics, principally for the measurement of the angular diameters of stars and for the measurement of binary star orbits.
	www.sciam.com /print_version.cfm?articleID=000B735C-8D98-1C72-9EB7809EC588F2D7 (2769 words)

	Why use an interferometer?
		When the interferometer is fully functioning as a precision astrometric instrument we expect to be able to measure star positions from the ground with an accuracy of about 1/1000 of a second of arc.
		Interferometers first became practical in the mid-1970s and are now under development in several parts of the world.
		One example of an interferometer is the NPOI on Anderson Mesa outside Flagstaff, Arizona.
	www.nofs.navy.mil /projects/npoi/whynpoi.htm (994 words)

	Three-Telescope Interferometer Shows Patchy Red Giants Common Fate Of Sun-Like Stars
		He found nearly one-third of the red giants he surveyed were not uniformly bright across their faces, but were patchy, perhaps indicating large spots or clouds analogous to sunspots, shock waves generated by pulsating envelopes, or even planets.
		Interferometers combine light from two or more telescopes to see more detail, simulating the resolution of a telescope as big as the distance between the telescopes.
		This contrasts with the typical interferometer, which consists of many mirrors to direct the light from multiple telescopes to a common detector.
	www.spacedaily.com /reports/Three_Telescope_Interferometer_Shows_Patchy_Red_Giants_Common_Fate_Of_Sun_Like_Stars_999.html (1546 words)

	Analog optical switch using an integrated Mach-Zehnder interferometer having a moveable phase shifter - Patent 6563965
		A Mach-Zehnder interferometer according to claim 1, wherein a surface is defined in said trench and wherein said phase shifter is selectively movable into and out of said second optical path along a line generally parallel with said surface.
		A Mach-Zehnder interferometer according to claim 1, wherein a surface is defined in said trench and wherein said phase shifter is selectively movable into and out of said second optical path along a line generally intersecting said surface.
		An optical signal propagating in and through the interferometer arm 17 will pass through phase shifter 51 or not, depending upon whether phase shifter 51 is positioned in or out of the optical path defined by and through that waveguide 117, trench 59 and waveguide 217.
	www.freepatentsonline.com /6563965.html (9414 words)

	29 July 2004: Cambridge and New Mexico astrophysicists take the next step towards world’s most ambitious optical ... (Site not responding. Last check: 2007-11-05)
		The Interferometer will be composed of several telescopes, spread out over an area larger than a football pitch and optically linked together to form a single ‘synthetic aperture’ 400 metres in diameter.
		The Interferometer will be a key feature of the Magdalena Ridge Observatory in New Mexico, which is being funded by the United States Congress, administered by the US Office of Naval Research and overseen by the US Naval Research Laboratory.
		The Cambridge team is led by Dr Chris Haniff and Dr David Buscher of the COAST Optical Interferometry Group at the Cavendish Laboratory, Cambridge.
	www.admin.cam.ac.uk /news/press/dpp/2004072901 (659 words)

	Adam Little \| Multiple Beam Interferometry Systems
		A basic interferometer is very simple in construction and can be quickly setup, the proper alignment of the system is typically the longest and most laborious portion of using an interferometer.
		The finesse factor is shown by the “sharpness” of the interferometer fringes.
		The finesse is directly related to the reflectivity of the interferometer cavity or the cavity of the etalon device.
	www.u.arizona.edu /~alittle/report.php (1320 words)

	[No title]
		The interferometer is of the Fizeau configuration with an aperture composed of twelve 1.2 meter mirrors on a 20 meter ring.
		Abstract: Space-based astrometric interferometer concepts typically have a requirement for the measurement of the internal dimensions of the instrument to accuracies in the picometer range.
		Also, when combining several laser interferometers to form a three- dimensional laser gauge (a laser optical truss), systematic errors due to imperfect knowledge of the truss geometry are important as the retroreflector translates away from its nominal zero-point.
	www.spie.org /web/abstracts/1900/1947.html (3803 words)

	The Ultimate 3C - American History Information Guide and Reference (Site not responding. Last check: 2007-11-05)
		The Third Cambridge Catalog of Radio Sources (3C) is an astronomical catalogue of celestial radio sources as measured at 159-MHz.
		It was published in 1959 by the Radio Astronomy Group of the University of Cambridge.
		The catalogue was produced by the Cambridge Interferometer on the west side of Cambridge.
	www.historymania.com /american_history/3C (234 words)

	400ft2.html
		The Cambridge instrument was a compound interferometer operating at 159 MHz.
		One of its problems involved misidentification of the reception lobes of the interferometer, thus causing ambiguities in source position.
		Laffineur had built an interferometer, each of whose elements was a 100-foot square (approximately) parabolic cylindrical reflector of poultry wire whose cylindrical axis was north-south.
	www.ece.uiuc.edu /pubs/reminisc/400ft/400ft2.html (581 words)

	Cambridge Consultants - CCL launches new SPR imaging technique, enabling high-throughput array-based analysis, ...
		Engineers at Cambridge Consultants Ltd (CCL) have developed a new system for the phase imaging of Surface Plasmon Resonance (SPR), enabling the high-throughput array-based analysis of molecular binding events, label-free.
		SPR has become widely used to characterise single biomolecular binding events, but there has been a real need for array-based analytical methods that can be used to detect such interactions without a requirement for molecular labelling.
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	www.cambridgeconsultants.com /news_pr76.shtml (656 words)

	Fabry-Perot Interferometer in an Optical Computer (Site not responding. Last check: 2007-11-05)
		The Fabry-Perot Interferometer was invented by French physicists Charles Fabry and Alfred Perot in 1897.
		The most basic form of a Fabry-Perot interferometer consists of two plane mirrors that are placed parallel to each other and separated by a space d.
		The main element of the optical transistor is the Fabry-Perot interferometer.
	www.u.arizona.edu /~bmj1/Report.htm (1328 words)

	2C: (Site not responding. Last check: 2007-11-05)
		The Second Cambridge Catalogue of Radio Sources (2C) was published in 1955 by John R Shakeshaft and colleagues.
		The observations were made with the Cambridge Interferometer, at 81.5 MHz.
		The 3C survey also used the Cambridge Interferometer, but at 159 MHz, which helped significantly reduce the 'confusion' (see above) in the later survey.
	winelib.com /wiki/2C (276 words)

	SPIE Proceedings Vol. 2477
		It comprises three stacked Fizeau interferometers viewing different directions within an instantaneous scanning circle, each interferometer consisting of two 50 cm aperture mirrors with a baseline separation of 2.5 m.
		The testbed is a full-scale model of a future space- based interferometer, containing all the spacecraft and support systems necessary to perform an astrometric measurement.
		Abstract: The Orbiting Stellar Interferometer (OSI) is a concept for a first-generation space interferometer with astrometric and imaging capabilities and its responsive to the recommendations of the Astronomy and Astrophysics Survey Committee for an astrometric interferometry mission.
	www.spie.org /web/abstracts/2400/2477.html (2778 words)

	COAST Home Page (Site not responding. Last check: 2007-11-05)
		COAST 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.
		VLTI, and future optical interferometer arrays, although limited astrophysical programmes are performed from time-to-time.
		Magdalena Ridge Observatory Interferometer (MROI), which will employ the principles pioneered at COAST to image faint and complex astronomical targets.
	www.mrao.cam.ac.uk /telescopes/coast (224 words)

	Events \| College of Optics & Photonics at the University of Central Florida
		The scientific rationale, how to directly detect a planet near a bright star, the optics of many types of coronagraphs, how to use its color and spectrum to characterize a planet, and how to search for life on a planet will be covered in this talk.
		The science and the optics and signal processing on how an interferometer works will be reviewed.
		(a) The IOTA interferometer uses 3 telescopes and integrated optics to combine the beams, all in the visible.
	www.creol.ucf.edu /TheCollege/EventDetail.aspx?EventID=35 (378 words)

	Radio telescope Summary
		In 1955, Sir Martin Ryle (1918-1984) invented the radio interferometer, a device in which several telescopes are linked to synthesize the performance of a single telescope with an extremely large aperture.
		In the early 1950s the Cambridge Interferometer mapped the radio sky to produce the famous 2C and 3C surveys of radio sources.
		In the late 1950s and early 1960s the largest single-dish radio telescope in the world was the 76 metre telescope at Jodrell Bank, which became operational in 1957.
	www.bookrags.com /Radio_telescope (1602 words)

	Fabry-Perot Interferometers - Cambridge University Press
		This book describes the Fabry-Perot interferometer and its variants as well as its use, optimisation and applications.
		However, there is also much practical detail on the use and optimization of the Fabry-Perot interferometer and discussion of its classical uses (such as in metrology) and its contemporary applications (such as in lasers).
		This book will appeal both to high-resolution practitioners, such as spectroscopists, and to the laser community, since the Fabrv-Perot is not only an integral part of the laser but is also usea to characterize its optical and spectroscopic behaviour.
	www.cambridge.org /catalogue/catalogue.asp?isbn=0521322383 (157 words)

	Physics at Minnesota: Physics and Astronomy Calendar
		The Magdalena Ridge Observatory Interferometer (MROI) is being designed and built at New Mexico Tech in collaboration with the University of Cambridge.
		The completed interferometer will be comprised of ten 1.4m telescopes in four scalable configurations, operating from 600 nm to 2.4 microns.
		We have several of the long lead-time components under contract and will be breaking ground on the interferometer buildings in late spring this year.
	www.physics.umn.edu /calendar/AC/calendar.html?item=1824 (169 words)

	[No title] (Site not responding. Last check: 2007-11-05)
		The observations were made with the Cambridge Interferometer, at 81.5 MHz.
		Unfortunately, this interpretation appears to have been premature - a significant number of the sources listed were later found to be the product of 'confusion', the blending of several weaker sources in the lobes of the interferometer to produce the apparent effect of a single stronger source.
		However, subsequent statistical analysis by Hewish of the interferometer records later showed some aspects of the initial interpretation to have been broadly correct.
	www.anime.co.za /wiki/2C (294 words)

	POINTS Abstracts
		Measurement at the microarcsec/year level of the apparent relative velocities of quasars that are widely separated on the sky severely test the assumption of cosmological quasar distances and may also constrain models of the early universe.
		POINTS, an astrometric optical interferometer with a nominal measurement accuracy of 5 microarcseconds for the angle between a pair of stars separated by about 90 deg, is presently under consideration.
		The purpose of the authors' research is to explore, from the point of view of nonlinear filtering, the feasibility of microarcsecond astrometry using space-based optical interferometers in typical disturbance environments.
	cfa-www.harvard.edu /~reasen/POINTS-abstracts.html (2554 words)

	The Comsic Background Imager
		Atmospheric emission increases the receiver noise, brightness fluctuations which are correlated between the antennas add noise at the correlator output, and path length fluctuations reduce the coherence.
		Path length fluctuations are caused by variations in the refractive index and are a problem for long baseline interferometers where the antennas look through different columns in the atmosphere.
		For short baseline interferometers, like the CBI, the antennas look through almost the same atmosphere so path length variations are small and the effects of atmospheric emission dominate.
	www.astro.caltech.edu /~tjp/cbidesc.html (4277 words)

	3C - TvWiki, the free encyclopedia (Site not responding. Last check: 2007-11-05)
		The Third Cambridge Catalogue of Radio Sources (3C) is an astronomical catalogue of celestial radio sources measured at 159-MHz.
		It was published in 1959 by the Radio Astronomy Group of the University of Cambridge.
		The catalogue was produced by the Cambridge Interferometer on the west side of Cambridge.
	www.tvwiki.tv /wiki/3C (276 words)

	Fourth Cambridge Survey of Radio Sources
		The Fourth Cambridge Radio Survey (4C) Catalogue contains all survey data from the papers of Pilkington and Scott (1965) and Gower, Scott and Wills (1967).
		These data result from a survey of radio sources between declinations -07 and +80 degrees using the large Cambridge interferometer at 178 MHz.
		The machine-readable version of the 4C catalog was received on magnetic tape from Dr. G.
	www.asc.rssi.ru /mdb/stars/8/8004.htm (913 words)

	LIGO - Laser Interferometer Gravitational Wave Observatory
		LHO receives the first Science Education Advocate Awards of Washington State LASER (Leadership and Assistance for Science Education Reform)...
		LCGT - The powerful next generation interferometer from Japan...
		Einstein@Home uses computer time donated by computer owners all over the world to process data from gravitational wave detectors...
	www.ligo.caltech.edu (114 words)

	Cambridge Interferometer - Wikipedia, the free encyclopedia
		The interferometer consisted of an array of 4 fixed elements to survey the sky.
		The telescope was operated by the Radio Astronomy Group of Cambridge University.
		Martin Ryle and Antony Hewish received the Nobel Prize for Physics in 1974 for this and other related work.
	en.wikipedia.org /wiki/Cambridge_Interferometer (125 words)

	David Buscher (Site not responding. Last check: 2007-11-05)
		I am a lecturer in the astrophysics group in the Cavendish Laboratory at Cambridge University.
		I work on the COAST optical/infrared interferometer in Cambridge and the MRO interferometer in New Mexico.
		The picture at the left is my face reflected in the deformable mirror of the ELECTRA adaptive optics system which I worked on in my previous job at Durham University.
	www.mrao.cam.ac.uk /~dfb/about.html (95 words)

	Catalogue: VIII/4
		VIII/4 Fourth Cambridge Survey (4C) (Pilkington+ 1965; Gower+ 1967) ================================================================================ A survey of radio sources between declinations 20 and 40.
		These data result from a survey of radio sources between declinations -07 and +80 degrees using the large Cambridge interferometer at 178 MHz.
		Remarks and Modifications: The machine-readable version of the 4C catalog was received on magnetic tape from Dr. G.
	cdsweb.u-strasbg.fr /viz-bin/Cat?VIII/4 (1140 words)

	New Mexico Tech and Cambridge sign major telescope agreement (Site not responding. Last check: 2007-11-05)
		The University of Cambridge and New Mexico Institute of Mining and Technology (New Mexico Tech) have signed a Memorandum of Understanding formalising their collaboration to build the Magdalena Ridge Observatory Interferometer, the world's most ambitious optical telescope array.
		The Memorandum was signed by the President of New Mexico Tech, Dr Daniel Lopez, and the head of the University of Cambridge’s Cavendish Laboratory, Professor Malcolm Longair, in the presence of University of Cambridge Vice-Chancellor Professor Alison Richard.
		For further information, please contact the University of Cambridge Office of Communications on 01223 332300
	www.admin.cam.ac.uk /news/dp/2004072901 (467 words)

	The Fourth Cambridge Survey of Radio Sources
		The Fourth Cambridge Radio Survey (4C) Catalogue contains all survey data from the papers of Pilkington and Scott (1965) and Gower, Scott and Wills (1967).
		The machine-readable version of the 4C catalog was received on magnetic tape from Dr. G.
		To distinguish them from published sources with blank class codes, a new numerical code of 15 was defined and added to the appropriate records.
	www.cs.wisc.edu /niagara/data/nasa/8004.xml (872 words)

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