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Radio telescope
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The 64-meter radio telescope at Parkes Observatory as seen in 1969, when it was used to receive live televised footage from Apollo 11
Antenna of UTR-2 low frequency radio telescope, Kharkiv region, Ukraine. Consists of an array of 2040 cage dipole elements.
A radio telescope is a specialized antenna and radio receiver used to receive radio waves from astronomical radio sources in the sky in radio astronomy.[1][2][3] Radio telescopes are the main observing instrument used in radio astronomy, which studies the radio frequency portion of the electromagnetic spectrum emitted by astronomical objects, just as optical telescopes are the main observing instrument used in traditional optical astronomy which studies the light wave portion of the spectrum coming from astronomical objects. Radio telescopes are typically large parabolic ("dish") antennas similar to those employed in tracking and communicating with satellites and space probes. They may be used singly or linked together electronically in an array. Unlike optical telescopes, radio telescopes can be used in the daytime as well as at night. Since astronomical radio sources such as planets, stars, nebulas and galaxies are very far away, the radio waves coming from them are extremely weak, so radio telescopes require very large antennas to collect enough radio energy to study them, and extremely sensitive receiving equipment. Radio observatories are preferentially located far from major centers of population to avoid electromagnetic interference (EMI) from radio, television, radar, motor vehicles, and other manmade electronic devices.
Radio waves from space were first detected by engineer Karl Guthe Jansky in 1932 at Bell Telephone Laboratories in Holmdel, New Jersey using an antenna built to study noise in radio receivers. The first purpose-built radio telescope was a 9-meter parabolic dish constructed by radio amateur Grote Reber in his back yard in Wheaton, Illinois in 1937. The sky survey he did with it is often considered the beginning of the field of radio astronomy.
Contents
[hide]
1 Early radio telescopes
2 Types
2.1 Frequencies
2.2 Big dishes
2.2.1 Gallery of big dishes
2.3 Radiotelescopes in space
3 Radio interferometry
4 Astronomical observations
5 See also
6 References
7 Further reading
8 External links
Early radio telescopes[edit]
Full-size replica of the first radio telescope, Jansky's dipole array, preserved at the US National Radio Astronomy Observatory in Green Bank, West Virginia.
Reber's first "dish" radio telescope - Wheaton, IL 1937
The first radio antenna used to identify an astronomical radio source was one built by Karl Guthe Jansky, an engineer with Bell Telephone Laboratories, in 1932. Jansky was assigned the job of identifying sources of static that might interfere with radio telephone service. Jansky's antenna was an array of dipoles and reflectors designed to receive short wave radio signals at a frequency of 20.5 MHz (wavelength about 14.6 meters). It was mounted on a turntable that allowed it to rotate in any direction, earning it the name "Jansky's merry-go-round". It had a diameter of approximately 100 ft (30 m) and stood 20 ft (6 m) tall. By rotating the antenna, the direction of the received interfering radio source (static) could be pinpointed. A small shed to the side of the antenna housed an analog pen-and-paper recording system. After recording signals from all directions for several months, Jansky eventually categorized them into three types of static: nearby thunderstorms, distant thunderstorms, and a faint steady hiss of unknown origin. Jansky finally determined that the "faint hiss" repeated on a cycle of 23 hours and 56 minutes. This period is the length of an astronomical sidereal day, the time it takes any "fixed" object located on the celestial sphere to come back to the same location in the sky. Thus Jansky suspected that the hiss originated outside of the Solar System, and by comparing his observations with optical astronomical maps, Jansky concluded that the radiation was coming from the Milky Way Galaxy and was strongest in the direction of the center of the galaxy, in the constellation of Sagittarius.
An amateur radio operator, Grote Reber, was one of the pioneers of what became known as radio astronomy. He built the first parabolic "dish" radio telescope, a 9 metres (30 ft) in diameter) in his back yard in Wheaton, Illinois in 1937. He repeated Jansky's pioneering work, identifying the Milky Way as the first off-world radio source, and he went on to conduct the first sky survey at very high radio frequencies, discovering other radio sources. The rapid development of radar during World War II created technology which was applied to radio astronomy after the war, and radio astronomy became a branch of astronomy, with universities and research institutes constructing large radio telescopes.[4]
Types[edit]
The range of frequencies in the electromagnetic spectrum that makes up the radio spectrum is very large. This means that the types of antennas that are used as radio telescopes vary widely in design, size, and configuration. At wavelengths of 30 meters to 3 meters (10 MHz - 100 MHz), they are generally either directional antenna arrays similar to "TV antennas" or large stationary reflectors with moveable focal points. 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.[5] [6] 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. Radio telescopes that operate at wavelengths of 3 meters to 30 cm (100 MHz to 1 GHz) are usually well over 100 meters in diameter. Telescopes working at wavelengths shorter than 30 cm (above 1 GHz) range in size from 3 to 90 meters in diameter.[citation needed]
Frequencies[edit]
The increasing use of radio frequencies for communication makes astronomical observations more and more difficult (see Open spectrum). Negotiations to defend the frequency allocation for parts of the spectrum most useful for observing the universe are coordinated in the Scientific Committee on Frequency Allocations for Radio Astronomy and Space Science.
Plot of Earth's atmospheric transmittance (or opacity) to various wavelengths of electromagnetic radiation.
Some of the more notable frequency bands used by radio telescopes include:
Every frequency in the United States National Radio Quiet Zone
Channel 37: 608 to 614 MHz
The "Hydrogen line", also known as the "21 centimeter line": 1420.40575177 MHz, used by many radio telescopes including The Big Ear in its discovery of the Wow! signal
1406 MHz and 430 MHz [7]
The Waterhole: 1,420 to 1,666 MHz
The Arecibo Observatory has several receivers that together cover the whole 1–10 GHz range.
The Wilkinson Microwave Anisotropy Probe mapped the Cosmic microwave background radiation in 5 different frequency bands, centered on 23 GHz, 33 GHz, 41 GHz, 61 GHz, and 94 GHz.
Big dishes[edit]
The world's largest filled-aperture (i.e. full dish) radio telescope is the Five hundred meter Aperture Spherical Telescope (FAST) completed in 2016 by China.[8] The 500-meter-diameter (1,600 ft) dish with an area as large as 30 football fields is built into a natural Karst depression in the landscape in Guizhou province and cannot move; the feed antenna is in a cabin suspended above the dish on cables. The active dish is composed of 4450 moveable panels controlled by a computer. By changing the shape of the dish and moving the feed cabin on its cables, the telescope can be steered to point to any region of the sky up to 40° from the zenith. Although the dish is 500 meters in diameter, only a 300-meter circular area on the dish is illuminated by the feed antenna at any given time, so the actual effective aperture is 300 meters. Construction was begun in 2007 and completed July 2016[9] and the telescope became operational September 25, 2016.[10]
The world's second largest filled-aperture telescope is the Arecibo radio telescope located in Arecibo, Puerto Rico. Another stationary dish telescope like FAST, whose 305 m (1,001 ft) dish is built into a natural depression in the landscape, the antenna is steerable within an angle of about 20° of the zenith by moving the suspended feed antenna. The largest individual radio telescope of any kind is the RATAN-600 located near Nizhny Arkhyz, Russia, which consists of a 576-meter circle of rectangular radio reflectors, each of which can be pointed towards a central conical receiver.
The above stationary dishes are not fully "steerable"; they can only be aimed at points in an area of the sky near the zenith, and cannot receive from sources near the horizon. The largest fully steerable dish radio telescope is the 100 meter Green Bank Telescope in West Virginia, United States, constructed in 2000. The largest fully steerable radio telescope in Europe is the Effelsberg 100-m Radio Telescope near Bonn, Germany, operated by the Max Planck Institute for Radio Astronomy, which also was the world's largest fully steerable telescope for 30 years until the Green Bank antenna was constructed.[11] The third-largest fully steerable radio telescope is the 76-meter Lovell Telescope at Jodrell Bank Observatory in Cheshire, England, completed in 1957. The fourth-largest fully steerable radio telescopes are six 70-meter dishes: three Russian RT-70, and three in the NASA Deep Space Network. As of 2016[update], the planned Qitai Radio Telescope will be the world's largest fully steerable single-dish radio telescope with a diameter of 110 m (360 ft).
A typical size of the single antenna of a radio telescope is 25 meters. Dozens of radio telescopes with comparable sizes are operated in radio observatories all over the world.
Gallery of big dishes[edit]
The 500 meter Five hundred meter Aperture Spherical Telescope (FAST), under construction, China (2016)
The 305 meter Arecibo Observatory, Puerto Rico (1963)
The 100 meter Green Bank Telescope, Green Bank, West Virginia, US, the largest fully steerable radio telescope dish (2002)
The 100 meter Effelsberg, in Bad Münstereifel, Germany (1971)
The 76 meter Lovell, Jodrell Bank Observatory, England (1957)
The 70 meter DSS 14 "Mars" antenna at Goldstone Deep Space Communications Complex, Mojave Desert, California, US (1958)
The 70 meter Yevpatoria RT-70, Crimea, first of three RT-70 in the former Soviet Union, (1978)
The 70 meter Galenki RT-70, Galenki, Russia, second of three RT-70 in the former Soviet Union, (1984)
The 70 meter DSS-43 antenna at Canberra Deep Space Communication Complex, Canberra, Australia (1987)
The 70 meter DSS-63 antenna at the Madrid Deep Space Communications Complex, near Madrid, Spain (late 1980s)
Radiotelescopes in space[edit]
Since 1965, humans have launched three space-based radio telescopes. In 1965, the Soviet Union sent the first one called Zond 3. In 1997, Japan sent the second, HALCA. The last one was sent by Russia in 2011 called Spektr-R.
Radio interferometry[edit]
Main article: Astronomical interferometer
See also: Radio astronomy § Radio interferometry
The Very Large Array in Socorro, New Mexico, an interferometric array formed of 27 parabolic dish telescopes.
One of the most notable developments came in 1946 with the introduction of the technique called astronomical interferometry, which means combining the signals from multiple antennas so that they simulate a larger antenna, in order to achieve greater resolution. Astronomical radio interferometers usually consist either of arrays of parabolic dishes (e.g., the One-Mile Telescope), arrays of one-dimensional antennas (e.g., the Molonglo Observatory Synthesis Telescope) or two-dimensional arrays of omnidirectional dipoles (e.g., Tony Hewish's Pulsar Array). All of the telescopes in the array are widely separated and are usually connected using coaxial cable, waveguide, optical fiber, or other type of transmission line. Recent advances in the stability of electronic oscillators also now permit interferometry to be carried out by independent recording of the signals at the various antennas, and then later correlating the recordings at some central processing facility. This process is known as Very Long Baseline Interferometry (VLBI). Interferometry does increase the total signal collected, but its primary purpose is to vastly increase the resolution through a process called Aperture synthesis. This technique works by superposing (interfering) the signal waves from the different telescopes on the principle that waves that coincide with the same phase will add to each other while two waves that have opposite phases will cancel each other out. This creates a combined telescope that is equivalent in resolution (though not in sensitivity) to a single antenna whose diameter is equal to the spacing of the antennas furthest apart in the array.
Atacama Large Millimeter Array in the Atacama desert consisting of 66 12-metre (39 ft), and 7-metre (23 ft) diameter radio telescopes designed to work at sub-millimeter wavelengths
A high-quality image requires a large number of different separations between telescopes. Projected separation between any two telescopes, as seen from the radio source, is called a baseline. For example, the Very Large Array (VLA) near Socorro, New Mexico has 27 telescopes with 351 independent baselines at once, which achieves a resolution of 0.2 arc seconds at 3 cm wavelengths.[12] Martin Ryle's group in Cambridge obtained a Nobel Prize for interferometry and aperture synthesis.[13] The Lloyd's mirror interferometer was also developed independently in 1946 by Joseph Pawsey's group at the University of Sydney.[14] In the early 1950s, the Cambridge Interferometer mapped the radio sky to produce the famous 2C and 3C surveys of radio sources. An example of a large physically connected radio telescope array is the Giant Metrewave Radio Telescope, located in Pune, India. The largest array, the Low-Frequency Array (LOFAR), is currently being constructed in western Europe, consisting of about 20,000 small antennas in 48 stations distributed over an area several hundreds of kilometers in diameter, and operates between 1.25 and 30 m wavelengths. VLBI systems using post-observation processing have been constructed with antennas thousands of miles apart. Radio interferometers have also been used to obtain detailed images of the anisotropies and the polarization of the Cosmic Microwave Background, like the CBI interferometer in 2004.
The world's largest physically connected telescopes, the Square Kilometre Array (SKA), are planned to start operation in 2024.
Astronomical observations[edit]
Main article: Radio astronomy
Many astronomical objects are not only observable in visible light but also emit radiation at radio wavelengths. Besides observing energetic objects such as pulsars and quasars, radio telescopes are able to "image" most astronomical objects such as galaxies, nebulae, and even radio emissions from planets.[citation needed]
See also[edit]
Aperture synthesis
Astropulse – distributed computing to search data tapes for primordial black holes, pulsars, and ETI
List of astronomical observatories
List of radio telescopes
List of telescope types
Search for extraterrestrial intelligence
Telescope
References[edit]
Jump up ^ Marr, Jonathan M.; Snell, Ronald L.; Kurtz, Stanley E. (2015). Fundamentals of Radio Astronomy: Observational Methods. CRC Press. pp. 21–24. ISBN 1498770193.
Jump up ^ Britannica Concise Encyclopedia. Encyclopædia Britannica, Inc. 2008. p. 1583. ISBN 1593394926.
Jump up ^ Verschuur, Gerrit (2007). The Invisible Universe: The Story of Radio Astronomy (2 ed.). Springer Science & Business Media. pp. 8–10. ISBN 0387683607.
Jump up ^ Sullivan, W.T. (1984). The Early Years of Radio Astronomy. Cambridge University Press. ISBN 0-521-25485-X
Jump up ^ Ley, Willy; Menzel, Donald H.; Richardson, Robert S. (June 1965). "The Observatory on the Moon". For Your Information. Galaxy Science Fiction. pp. 132–150.
Jump up ^ CSIRO. "The Dish turns 45". Commonwealth Scientific and Industrial Research Organisation. Archived from the original on August 24, 2008. Retrieved October 16, 2008.
Jump up ^ "Microstructure". Jb.man.ac.uk. 1996-02-05. Retrieved 2016-02-24.
Jump up ^ "China Exclusive: China starts building world's largest radio telescope - People's Daily Online". English.peopledaily.com.cn. 2008-12-26. Retrieved 2016-02-24.
Jump up ^ "China Finishes Building World's Largest Radio Telescope". 2016-07-06. Retrieved 2016-07-06.
Jump up ^ Wong, Gillian (25 September 2016), China Begins Operating World's Largest Radio Telescope, ABC News
Jump up ^ Ridpath, Ian (2012). A Dictionary of Astronomy. OUP Oxford. p. 139. ISBN 0-19-960905-5.
Jump up ^ "Microwave Probing of the Invisible". Archived from the original on August 31, 2007. Retrieved June 13, 2007.
Jump up ^ Nature vol.158, p. 339, 1946
Jump up ^ Nature vol.157, p.158, 1946
Further reading[edit]
Wikimedia Commons has media related to Radio telescopes.
Rohlfs, K., & Wilson, T. L. (2004). Tools of radio astronomy. Astronomy and astrophysics library. Berlin: Springer.
Asimov, I. (1979). Isaac Asimov's Book of facts; Sky Watchers. New York: Grosset & Dunlap. Page 390 - 399. ISBN 0-8038-9347-7
External links[edit]
astronomytoday.com - "Radio Astronomy" by Sancar J Fredsti
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Radio astronomy
Concepts
Astronomical interferometer (History)
Very Long Baseline Interferometry (VLBI)
Radio telescope (Radio window)
Astronomical radio source
Units (watt and jansky)
Radio telescopes (List)
Individual telescopes
RATAN-600 Radio Telescope (Russia)
500 m Aperture Spherical Telescope (FAST, China)
Arecibo Observatory (Puerto Rico, US)
Caltech Submillimeter Observatory (CSO, US)
Effelsberg Telescope (Germany)
Large Millimeter Telescope (Mexico)
Yevpatoria RT-70 (Ukraine)
Galenki RT-70 (Russia)
Suffa RT-70 (Uzbekistan)
Green Bank Telescope (West Virginia, US)
Lovell Telescope (UK)
Ooty Telescope (India)
UTR-2 decameter radio telescope (Ukraine)
Sardinia Radio Telescope (Italy)
Usuda Telescope (Japan)
Qitai Radio Telescope (China)
Southern Hemisphere
HartRAO (South Africa)
Parkes Observatory (Australia)
Warkworth Radio Astronomical Observatory (NZ)
Interferometers
Allen Telescope Array (ATA, California, US)
Atacama Large Millimeter Array (ALMA, Chile)
Australia Telescope Compact Array (ATCA, Australia)
Australian Square Kilometre Array Pathfinder (ASKAP, Australia)
Canadian Hydrogen Intensity Mapping Experiment (CHIME, Canada)
Combined Array for Research in Millimeter-wave Astronomy (CARMA, California, US)
European VLBI Network (Europe)
Event Horizon Telescope (EHT)
Green Bank Interferometer (GBI, West Virginia, US)
Giant Metrewave Radio Telescope (GMRT, India)
Korean VLBI Network (KVN, South Korea)
Low-Frequency Array (LOFAR, Netherlands)
MeerKAT (South Africa)
Large Latin American Millimeter Array (LLAMA, Argentina/Brazil)
Murchison Widefield Array (MWA, Australia)
Multi-Element Radio Linked Interferometer Network (MERLIN, UK)
Molonglo Observatory Synthesis Telescope (MOST, Australia)
Northern Cross Radio Telescope (Italy)
Northern Extended Millimeter Array (France)
One-Mile Telescope (UK)
Primeval Structure Telescope (PaST, China)
Square Kilometre Array (SKA, Australia, South Africa)
Submillimeter Array (SMA, US)
Very Large Array (VLA, New Mexico, US)
Very Long Baseline Array (VLBA, US)
Westerbork Synthesis Radio Telescope (WSRT, Netherlands)
Space-based telescopes
Spektr-R (Russia)
HALCA (Japan)
Observatories
Algonquin Radio Observatory (Canada)
Haystack Observatory (US)
Jodrell Bank Observatory (UK)
Mullard Radio Astronomy Observatory (UK)
National Radio Astronomy Observatory (US)
Onsala Space Observatory (Sweden)
Special Astrophysical Observatory of the Russian Academy of Science (SAORAS, Russia)
Warkworth Radio Astronomical Observatory
Pushchino Radio Astronomy Observatory (PRAO ASC LPI, Russia)
Multi-use
PARL (Canada)
DRAO (Canada)
ESA New Norcia (Australia)
People
Elizabeth Alexander
John G. Bolton
Edward George Bowen
Ronald Bracewell
Jocelyn Bell Burnell
Arthur Covington
Frank Drake
Antony Hewish
Karl Guthe Jansky (Unit: jansky)
Kenneth Kellermann
Frank J. Kerr
John D. Kraus
Bernard Lovell
Jan Oort
Joseph Lade Pawsey
Ruby Payne-Scott
Arno Penzias
Govind Swarup
Grote Reber
Martin Ryle
Gart Westerhout
Paul Wild
Robert Wilson
Related articles
Cosmic microwave background radiation
SETI
Interferometry
Radio propagation
Aperture synthesis
Wow! signal
Radio signal from HD 164595
Pulsar timing array
Optical astronomy
Submillimetre astronomy
Infrared astronomy
High-energy astronomy
Gravitational-wave astronomy
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values: റേഡിയോ ദൂരദർശിനി – Malayalam

values:
interlanguage-link interwiki-ml
display: none;

values: रेडिओ दुर्बीण – Marathi

values:
interlanguage-link interwiki-mr
display: none;

values:
interlanguage-link interwiki-nl
display: none;

values:
interlanguage-link interwiki-ja
display: none;

values:
interlanguage-link interwiki-no
display: none;

values:
interlanguage-link interwiki-nn
display: none;

values:
interlanguage-link interwiki-uz
display: none;

values:
interlanguage-link interwiki-pl
display: none;

values:
interlanguage-link interwiki-ro
display: none;

values: Радиотелескоп – Russian

values:
interlanguage-link interwiki-stq
display: none;

values:
interlanguage-link interwiki-sq
display: none;

values:
interlanguage-link interwiki-simple
display: none;

values:
interlanguage-link interwiki-sk
display: none;

values: Радио-телескоп – Serbian

values:
interlanguage-link interwiki-sr
display: none;

values:
interlanguage-link interwiki-sh
display: none;

values:
interlanguage-link interwiki-fi
display: none;

values:
interlanguage-link interwiki-sv
display: none;

values: வானொலி அதிர்வெண் தொலைநோக்கி – Tamil

values:
interlanguage-link interwiki-ta
display: none;

values: กล้องโทรทรรศน์วิทยุ – Thai

values:
interlanguage-link interwiki-th
display: none;

values:
interlanguage-link interwiki-tr
display: none;

values: Радіотелескоп – Ukrainian

values:
interlanguage-link interwiki-uk
display: none;

values:
interlanguage-link interwiki-vi
display: none;

values: All languages (initial selection from common choices by you and others)

values: /static/images/wikimedia-button-1.5x.png 1.5x, /static/images/wikimedia-button-2x.png 2x

values: /static/images/poweredby_mediawiki_132x47.png 1.5x, /static/images/poweredby_mediawiki_176x62.png 2x

values:
suggestions
display: none; font-size: 13px;

values: mediawiki ltr sitedir-ltr mw-hide-empty-elt ns-0 ns-subject page-Radio_telescope rootpage-Radio_telescope skin-vector action-view