Difference between revisions 1434860 and 1435034 on enwikiversity

[[Image:Brorfelde Schmidt Telescope.jpg|thumb|right|200px|The Schmidt Telescope at the former Brorfelde Observatory is now used by amateur astronomers. Credit: [[commons:User:Moeng|Mogens Engelund]].]]
A '''radiation telescope''' is an instrument designed to collect and focus radiation so as to make distant sources appear nearer.
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=[[Astronomy]]=
(contracted; show full)|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=December 8,
|year=2012
|url=http://en.wikipedia.org/wiki/Astronomical_spectroscopy
|accessdate=2013-01-09 }}</ref>

=
Spectrometers[[Radiation astronomy/Spectrometers|Spectrometers]]=
[[Image:Osse.gif|thumb|right|200px|The Oriented Scintillation Spectrometer Experiment (OSSE) consists of four NaI scintillation detectors, sensitive to energies from 50 keV to 10 MeV. Credit: NASA GSFC.]]
"The Oriented Scintillation Spectrometer Experiment (OSSE) will conduct a broad range of observations in the 0.05-250 MeV energy range. Major emphasis is placed on scientific objectives in the 0.1-10.0 MeV region with a limited capability above 10 MeV, primarily for observations of solar gamma-rays and neutrons and observations of high-energy emission from pulsars."<ref name=Johnson>{{ cite web
|author=W. N. Johnson
|title=Appendix G to the NASA RESEARCH ANNOUNCEMENT for the COMPTON GAMMA RAY OBSERVATORY GUEST INVESTIGATOR PROGRAM
|publisher=National Aeronautics and Space Administration Goddard Space Flight Center
|location=Greenbelt, Maryland USA
|month=November
|year=1996
|url=http://heasarc.gsfc.nasa.gov/docs/cgro/nra/appendix_g.html#III.%20COMPTEL%20GUEST%20INVESTIGATOR%20PROGRAM
|accessdate=2013-04-05 }}</ref>
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=[[Instruments/Telescopes/Planetary|Planetary telescopes]]=
[[Image:Goto telescope.jpg|thumb|right|A telescope on an alt-azimuth GoTo mount.  Note the keypad, resting on the platform between the tripod's legs, that is the telescope's hand control.  Batteries are stored in the circular compartment just above the tripod.  In this picture, the compartment is just above the hand control.]]
"In [[amateur astronomy]], "'''GoTo'''" refers to a type of [[telescope mount]] and related [[software]] which can automatically point a telescope to [[astronomical objects]] that the user selects. Both axes of a GoTo mount are motor driven and are controlled by either a microprocessor-based integrated controller or a personal computer, as opposed to the single axis semi-automated tracking of a traditional clock drive mount. This allows the user to command the mount to point the telescope to a right ascension and declination that the user inputs or have the mount itself point the telescope to objects in a pre-programmed data base including ones from the Messier catalogue, the New General Catalogue, and even major solar system bodies (the Sun, Moon, and planets)."<ref name=GoToTelescopes>{{ cite web
|title=GoTo (telescopes), In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=May 27.
|year=2013
|url=https://en.wikipedia.org/wiki/GoTo_(telescopes)
|accessdate=2014-01-03 }}</ref>
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=[[Instruments/Telescopes/Solar|Solar telescopes]]=
[[Image:Kitt Peak McMath-Pierce Solar Telescope.jpg|thumb|right|200px|This view is of the McMath-Pierce Solar Telescope at Kitt Peak National Observatory, near Tucson, Arizona. Credit: [http://www.flickr.com/photos/oceanyamaha/ ocean yamaha].]]
"A '''solar telescope''' is a special purpose [[w:telescope|telescope]] used to observe the [[Sun (star)|Sun]]. Solar telescopes usually detect light with wavelengths in, or not far outside, the [[w:visible spectrum|visible spectrum]]."<ref name=SolarTelescope>{{ cite web
|title=Solar telescope, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=May 31,
|year=2012
|url=http://en.wikipedia.org/wiki/Solar_telescope
|accessdate=2012-07-07 }}</ref>
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=[[Instruments/Telescopes/Asteroids|Asteroid telescopes]]=
[[Image:Lowell astrograph.jpg|thumb|200px|right|The Lowell astrograph is a dedicated astrophotography telescope. Credit: .]]
The Lowell astrograph imaged at right is a 13-inch, f/5.3 astrograph at Lowell Observatory,  a refractor with a 3 element Cooke triplet lens.<ref name=Tombaugh>{{ cite web
|author=Clyde W. Tombaugh
|title=The Struggles to Find the Ninth Planet
|url=http://ircamera.as.arizona.edu/NatSci102/NatSci102/text/ext9thplanet.htm }}</ref>) that was used in the discovery of [[Pluto]].

"An '''astrograph''' ('''astrographic camera''') is a telescope designed for the sole purpose of astrophotography. Astrographs are usually used in wide field surveys of the night sky as well as detection of objects such as [[asteroids]], [[meteor]]s, and [[comet]]s."<ref name=Astrograph>{{ cite web
|title=Astrograph, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=December 12,
|year=2013
|url=https://en.wikipedia.org/wiki/Astrograph
|accessdate=2014-01-03 }}</ref>
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=Comet [[Instruments/Telescopes/Comet seekers|Comet-seeker telescopes]]=

"A comet seeker is a type of small telescope adapted especially to searching for comets: commonly of short focal length and large aperture, in order to secure the greatest brilliancy of light."<ref name=CometSeeker>{{ cite web
|title=Comet seeker, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=March 6,
|year=2013
|url=https://en.wikipedia.org/wiki/Comet_seeker
|accessdate=2014-01-03 }}</ref>

=[[Instruments/Telescopes/Stars|Stellar telescopes]]=
[[File:FASTT Transit Circle.jpg|thumb|right|200px|The Ron Stone/Flagstaff Astrometric Scanning Transit Telescope of the U.S.Naval Observatory, built by Farrand Optical Company, 1981, is imaged. Credit: .]]
(contracted; show full)|first2=David G.
|last2=Monet
|year=1990
|journal=Proceedings of IAU Symposium No. 141
|pages=369–370 }}</ref>"<ref name=MeridianCircle/>
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=
[[Instruments/Telescopes/Galaxies|Galactic telescopes]]=
[[Image:NGC 891 HST.jpg|thumb|right|200px|NGC 891 is selected as first light. Credit: NASA.]]
[[Image:LargeBinoTelescope NASA.jpg|thumb|left|200px|This is an image of the Large Binocular Telescope with protective doors open. Credit: NASA.]]
The Large Binocular Telescope [at left] is "located on Mount Graham (10,700-foot (3,300 m)) in the Pinaleno Mountains of southeastern Arizona, and is a part of the Mount Graham International Observatory."<ref name=LargeBinocularTelescope>{{ cite web
|title=Large Binocular Telescope, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=May 21,
|year=2013
|url=http://en.wikipedia.org/wiki/Large_Binocular_Telescope
|accessdate=2013-07-02 }}</ref>

"The first image taken [shown at right] combined ultraviolet and green light, and emphasizes the clumpy regions of newly formed hot stars in the spiral arms."<ref name=LargeBinocularTelescope/>
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=[[Geography/Earth/Locations|Locations on Earth]]=
[[Image:VERITAS array.jpg|thumb|right|300px|VERITAS is located at the basecamp of the Smithsonian Astrophysics Observatory's Fred Lawrence Whipple Observatory (FLWO) in southern Arizona. Credit: VERITAS.]]
[[Image:Aerial View of the VLTI with Tunnels Superimposed.jpg|200px|thumb|left|The four Unit Telescopes form the VLT together with the Auxiliary Telescopes. Credit: .]]
"VERITAS (Very Energetic Radiation Imaging Telescope Array System) is a ground-based gamma-ray instrument operating at the Fred Lawrence Whipple Observatory (FLWO) in southern Arizona, USA. It is an array of four 12m optical reflectors for gamma-ray astronomy in the GeV - TeV energy range. These imaging Cherenkov [a bluish light] telescopes are deployed such that they have the highest sensitivity in the VHE energy band (50 GeV - 50 TeV), with maximum sensitivity from 100 GeV to 10 TeV. This VHE observatory effectively complements the NASA Fermi mission."<ref name=Fortin>{{ cite web
|author=Pascal Fortin
|title=VERITAS Very Energetic Radiation Imaging Telescope Array System
|publisher=Smithsonian Astrophysical Observatory
|location=Amado, Arizona USA
|month=April 14
|year=2013
|url=http://veritas.sao.arizona.edu/
|pdf=⏎
|accessdate=2013-06-01 }}</ref>

The Collaboration between Australia and Nippon for a Gamma Ray Observatory in the Outback, (CANGAROO) is for "[v]ery high energy cosmic gamma ray observation by telescope [detecting Cherenkov light]. [It is] [l]ocated on the [[w:Woomera Prohibited Area|Woomera Prohibited Area]] in South Australia. <ref name=CANGAROO>{{ cite web
|url=http://www.physics.adelaide.edu.au/astrophysics/cangaroo/index.html
|title=The CANGAROO Project
(contracted; show full)|location=San Francisco, California
|month=June 17,
|year=2013
|url=http://en.wikipedia.org/wiki/Very_Large_Telescope
|accessdate=2013-07-02 }}</ref>
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=
[[History/Recent|Recent history]]=
[[Image:TransitCircle USNO.jpg|thumb|right|200px|This is the 6-inch transit circle of the U.S. Naval Observatory. Credit: .]]
The '''recent history''' period dates from around 1,000 b2k to present.⏎
⏎
The 6-inch transit circle [imaged at right] of the U.S. Naval Observatory was built by Warner and Swasey in 1898.
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=Apertures[[Radiation astronomy/Telescopes/Apertures|Coded apertures]]=

"Some X-ray telescopes use coded aperture imaging. This technique uses a flat aperture grille in front of the detector, which weighs much less than any kind of focusing X-ray lens, but requires considerably more post-processing to produce an image."<ref name=XRayTelescope>{{ cite web
|title=X-ray telescope, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=April 17,
|year=2012
|url=http://en.wikipedia.org/wiki/X-ray_telescope
|accessdate=2012-06-15 }}</ref>

=Mirrors[[Radiation astronomy/Telescopes/Mirrors|Mirrors]]=
[[Image:Wolter-types.gif|thumb|right|200px|This is a diagram of Wolter telescopes of Types I, II, and III. Credit: .]]
"The mirrors can be made of ceramic or metal foil.<ref name=xraysMirror>{{ cite web |title=Mirror Laboratory |url=http://astrophysics.gsfc.nasa.gov/xrays/MirrorLab/xoptics.html }}</ref> The most commonly used grazing angle incidence materials for X-ray mirrors are [[w:gold|gold]] and [[w:iridium|iridium]]. The critical reflection angle is energy dependent. For gold at 1&a(contracted; show full)|location=San Francisco, California
|month=June 10,
|year=2012
|url=http://en.wikipedia.org/wiki/History_of_the_telescope
|accessdate=2012-06-26 }}</ref>
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=
Modulation collimators[[Radiation astronomy/Telescopes/Modulation collimators|Modulation collimators]]=
[[Image:Four-wire grid modulation collimator.jpeg|thumb|right|200px|The diagram shows the principles of operation of the four-grid modulation collimator. Credit: H. Bradt, G. Garmire, M. Oda, G. Spada, and B.V. Sreekantan, P. Gorenstein and H. Gursky.]]
A modulation collimator consists of “two or more wire grids [diffraction gratings] placed in front of an X-ray sensitive Geiger tube or proportional counter.”<ref name=Bradt>{{ cite journal
|author=H. Bradt, G. Garmire, M. Oda, G. Spada, and B.V. Sreekantan, P. Gorenstein and H. Gursky
|title=The Modulation Collimator in X-ray Astronomy
|journal=Space Science Reviews
|month=September
|year=1968
|volume=8
|issue=4
|pages=471-506
|url=
|arxiv=
|bibcode=1968SSRv....8..471B
|doi=10.1007/BF00175003
|pmid=
|pdf=⏎
|accessdate=2011-12-10 }}</ref> Relative to the path of incident X-rays (incoming X-rays) the wire grids are placed one beneath the other with a slight offset that produces a shadow of the upper grid over part of the lower grid.<ref name=Oda>{{ cite journal
|author=Minoru Oda
|title=High-Resolution X-Ray Collimator with Broad Field of View for Astronomical Use
|journal=Applied Optics
|month=January
|year=1965
|volume=4
|issue=1
|pages=143
|url=http://www.opticsinfobase.org/abstract.cfm?URI=ao-4-1-143
|arxiv=
|bibcode=1965ApOpt...4..143O
|doi=10.1364/AO.4.000143
|pmid=
|pdf=http://www.opticsinfobase.org/ao/viewmedia.cfm?uri=ao-4-1-143&seq=0
|accessdate=2011-12-10 }}</ref>
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=[[Computers]]=
[[Image:Lights glowing on the ALMA correlator.jpg|thumb|right|200px|The ALMA correlator is one of the most powerful supercomputers in the world. Credit: ALMA (ESO/NAOJ/NRAO), S. Argandoña.]]
"The ALMA correlator [shown at right], one of the most powerful supercomputers in the world, has now been fully installed and tested at its remote, high altitude site in the Andes of northern Chile. This view shows lights glowing on some of the racks of the correlator in the ALMA Array Operations Site Techical Building. This photograph shows one of the four quadrants of the correlator. The full system has four identical quadrants, with over 134 million processors, performing up to 17 quadrillion operations per second."<ref name=ALMAObservatory>{{ cite web
|author=ALMA Observatory
|title=Lights glowing on the ALMA correlator
|publisher=ALMA Observatory Organization
|location=Atacama, chile
|month=July 10,
|year=2013
|url=http://www.almaobservatory.org/en/visuals/images/the-alma-observatory/?g2_itemId=3939
|pdf=⏎
|accessdate=2013-07-21 }}</ref>
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=Mounts[[Instruments/Telescopes/Mounts|Telescope mounts]]=

“A telescope mount is a mechanical structure which supports a telescope. Telescope mounts are designed to support the mass of the telescope and allow for accurate pointing of the instrument.”<ref name=Telescope>{{ cite web
|title=Telescope, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=July 4,
|year=2012
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=Hexapod mounts=
[[Image:DOT main mirror.jpg|thumb|right|200px|This is an image of the top part of the Dutch Open Telescope. Credit: Tim van Werkhoven.]]
“Instead of the classical mounting using two axles, the mirror is supported by six extendable struts (hexapod). This configuration allows moving the telescope in all six spatial degrees of freedom and also provides a strong structural integrity.”<ref name=TelescopeMount/>
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=
[[Clocks/Drives|Clock drives]]=
[[Image:Aldershot observatory 02.JPG|thumb|right|200px|The clock drive mechanism in the pier of the german equatorial mount for the 8-inch refracting telescope at [[w:Aldershot Observatory|Aldershot Observatory]] is shown in the image. Credit: .]]
(contracted; show full)|location=San Francisco, California
|month=May 30,
|year=2012
|url=http://en.wikipedia.org/wiki/Clock_drive
|accessdate=2012-07-07 }}</ref>
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=
[[Clocks]]=
[[Image:FOCS-1.jpg|thumb|left|200px| The FOCS 1 is a continuous cold caesium fountain atomic clock in Switzerland. Credit: .]]
"An '''atomic clock''' is a [[w:clock|clock]] device that uses an [[w:electronic transition|electronic transition]] [[w:frequency|frequency]] in the [[w:microwave|microwave]], [[w:light|optical]], or [[w:ultraviolet|ultraviolet]] region<ref name=McCarthy>{{ cite book
|title=TIME from Earth Rotation to Atomic Physics
(contracted; show full)|year=2012
|url=http://en.wikipedia.org/wiki/Atomic_clock
|accessdate=2012-10-24 }}</ref>

The FOCS 1 continuous cold cesium fountain atomic clock started operating in 2004 at an uncertainty of one second in 30 million years. The clock is in Switzerland.
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=
[[Motion calibrators]]=

"'''POA CALFOS''' is the improved Post Operational Archive version of the [[w:Faint Object Spectrograph|Faint Object Spectrograph]] (FOS) calibration pipeline ... The current version corrects for image motion problems that have led to significant wavelength scale uncertainties in the FOS data archive. The improvements in the calibration enhance the scientific value of the data in the FOS archive, making it a more homogeneous and reliable resource."<ref name=POACALFOS>{{ cite web
|title=POA CALFOS, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=July 22
|year=2012
|url=http://en.wikipedia.org/wiki/POA_CALFOS
|accessdate=2012-12-23 }}</ref>

=Detectors[[Radiation astronomy/Detectors|Detectors]]=
[[Image:Proportional Counter Array RXTE.jpg|thumb|right|200px|This is an image of a real X-ray detector. The instrument is called the Proportional Counter Array and it is on the [[w:Rossi X-ray Timing Explorer|Rossi X-ray Timing Explorer]] (RXTE) satellite. Credit: .]]
"[[Radiation detectors]] provide a signal that is converted to an electric current. The device is designed so that the current provided is proportional to the characteristics of the incident radiation."<ref name=RadiationDetectors>{{ cite web
|title=Radiation detectors, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=June 19,
|year=2012
|url=http://en.wikiversity.org/wiki/Radiation_detectors
|accessdate=2012-07-07 }}</ref>

Detectors such as the X-ray detector at right collect individual X-rays (photons of X-ray light), count them, discern the energy or wavelength, or how fast they are detected. The detector and telescope system can be designed to yield temporal, spatial, or spectral information.
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=Image processors[[Instruments/Telescopes/Image processors|Image processors]]=

'''Def.''' “[a]ny form of information processing for which both the input and output are images”, after Wiktionary [[wikt:image processing|image processing]], is called '''image processing'''.

'''Def.''' “[a] representation of anything ... upon canvas, paper, or other surface”, after Wiktionary [[wikt:picture|picture]], is called a '''picture'''.

(contracted; show full) | title = Principles of Optics
  | publisher = Cambridge University Press
  | date = October 1999
  | location = Cambridge
  | page = 461
  | isbn = 0-521-64222-1}}</ref>"<ref name=AngularResolution/>

=
[[Instruments/Telescopes/Robotics|Robotic telescopes]]=
[[Image:El Enano robotic telescope.jpg|thumb|right|200px|“El Enano” is a robotic telescope. Credit: .]]
"A '''robotic telescope''' is an astronomical telescope and detector system that makes observations without the intervention of a human. In astronomical disciplines, a telescope qualifies as robotic if it makes those observations without being operated by a human, even if a human has to initiate the observations at the beginning of the night, or end them in the morning. A robotic telescope is distinct from a remote telescope, though an instrument can be both robotic and remote."<ref name=RoboticTelescope>{{ cite web
|title=Robotic telescope, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=July 1,
|year=2013
|url=https://en.wikipedia.org/wiki/Robotic_telescope
|accessdate=2014-01-03 }}</ref>
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=[[Instruments/Telescopes/Spotting|Spotting telescopes]]=
[[Image:Yukon spotting scope.jpg|thumb|right|200px|This is a 100 mm spotting scope with a coaxial 30 mm finderscope. Credit: .]]
"A '''spotting scope''' is a small portable [[telescope]] with added optics to present an [[erect image]], optimized for the observation of terrestrial objects."<ref name=SpottingScope>{{ cite web
|title=article title, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=February 28,
|year=2013
|url=https://en.wikipedia.org/wiki/Spotting_scope
|accessdate=2014-01-03 }}</ref>

"The light-gathering power and [angular] resolution of a spotting scope is determined by the diameter of the objective lens, typically between 50 and 80 mm. The larger the objective, the more massive and expensive the telescope."<ref name=SpottingScope/>

"The optical assembly has a small refracting objective lens, an image erecting system that uses either image erecting relay lenses or prisms (porro prisms or roof prisms), and an eyepiece that is usually removable and interchangeable to give different magnifications. Other telescope designs are used such as Schmidt and Maksutov optical assemblies. They may have a ruggedised design, a mounting for attaching to a tripod, and an ergonomically designed and located knob for focus control."<ref name=SpottingScope/>
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=[[Astronomy/Observatories|Observatories]]=
[[Image:Champaign-Urbana area IMG 1138.jpg|right|thumb|200px|This equatorial room is at the University of Illinois Observatory. Credit: .]]
"Historically, observatories [are] as simple as [using or placing stably] an astronomical sextant (for measuring the distance between stars) or Stonehenge (which has some alignments on astronomical phenomena). ... Most optical telescopes are housed within a dome or similar structure, to protect the delicate instruments from the elements. Telescope domes have a sl(contracted; show full)|location=San Francisco, California
|month=May 14,
|year=2012
|url=http://en.wikipedia.org/wiki/Equatorial_room
|accessdate=2012-07-07 }}</ref>
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=
[[Lofting technology]]=

Many devices for lofting technology have been developed to improve [[radiation astronomy]].

=Balloons[[Astronomy/Balloons|Balloons]]=
[[Image:BLAST on flightline kiruna 2005.jpeg|thumb|right|200px|BLAST is hanging from the launch vehicle in [[w:Esrange|Esrange]] near [[w:Kiruna|Kiruna]], [[w:Sweden|Sweden]] before launch June 2005. Credit: [[commons:User:Mtruch|Mtruch]].]]
(contracted; show full)|location=McMurdo Station
|month=December 26,
|year=2012
|url=http://news.yahoo.com/nasa-launches-telescope-toting-balloon-antarctica-christmas-164200686.html
|accessdate=2012-12-26 }}</ref>
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=
[[Astronomy/Airborne/Launches|Aircraft assisted launches]]=

"The '''Array of Low Energy X-ray Imaging Sensors''' ('''ALEXIS''') [[X-ray astronomy|X-ray]] telescopes feature curved mirrors whose multilayer coatings reflect and focus low-energy X-rays or extreme ultraviolet light the way [[w:optical telescope|optical telescope]]s focus visible light. ... The Launch was provided by the [[w:United States Air Force|United States Air Force]] Space Test Program on a [[w:Pegasus rocket|Pegasus]] Booster on April 25, 1993.<ref name=ALEXIA>{{ cite web
|title=ALEXIS satellite marks fifth anniversary of launch
|url=http://www.fas.org/spp/military/program/masint/98-062.html
|accessdate=17 August 2011
|publisher=Los Alamos National Laboratory
|date=23 April 1998 }}</ref>"<ref name=ALEXIS>{{ cite web
|title=Array of Low Energy X-ray Imaging Sensors, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=December 18,
|year=2011
|url=http://en.wikipedia.org/wiki/Array_of_Low_Energy_X-ray_Imaging_Sensors
|accessdate=2012-12-09 }}</ref>

=[[Research]]=

Hypothesis:⏎
# Ancients had and used telescopes.

==[[Control groups]]==
[[Image:Lewis rat.jpg|thumb|right|200px|This is an image of a Lewis rat. Credit: Charles River Laboratories.]]
The findings demonstrate a statistically systematic change from the ''status quo'' or the control group.

“In the design of experiments, treatments [or special properties or characteristics] are applied to [or observed in] experimental units in the '''treatment group'''(s).<ref name=Hinkelmann>{{ cite book
(contracted; show full)|bibcode=
|doi=10.1016/S0140-6736(05)67098-5
|pmid=
|accessdate=2012-05-09 }}</ref>

Proof of concept consists of a prototype instrument or device that makes a distant source appear nearer.

==
[[Proof of technology]]==

"[T]he objective of a proof of technology is to determine the solution to some technical problem, such as how two systems might be integrated or that a certain throughput can be achieved with a given configuration."<ref name=ProofofConcept>{{ cite web
|title=Proof of concept, In: ''Wikipedia''
|publisher=Wikimedia Foundation, Inc
|location=San Francisco, California
|month=December 27,
|year=2012
(contracted; show full)[[Category:Original research]]
[[Category:Physics and Astronomy]]
[[Category:Research]]
[[Category:Resources last modified in February 2015]]
[[Category:Technology]]
{{experimental}}{{article}}{{lecture}}{{astronomy}}{{Materials science}}{{technology}}

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