716:
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20:
802:
468:
786:
388:
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183:
35:
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1002:(LOFAR), finished in 2012, is located in western Europe and consists of about 81,000 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
319:
2560:
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2510:
254:(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
2536:
2572:
616:
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632:
770:
508:
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 and the telescope became operational
September 25, 2016.
367:
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
507:
is in a cabin suspended above the dish on cables. The active dish is composed of 4,450 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.
915:
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.
527:); most other telescopes employ passive detection, i.e., receiving only. Arecibo was another stationary dish telescope like FAST. Arecibo's 305 m (1,001 ft) dish was built into a natural depression in the landscape, the antenna was steerable within an angle of about 20° of the
298:. He built the first parabolic "dish" radio telescope, 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
715:
891:. 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
121:
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 telescopes are typically large
856:, 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
695:
258:
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 above
346:
arrays similar to "TV antennas" or large stationary reflectors with movable focal points. Since the wavelengths being observed with these types of antennas are so long, the "reflector" surfaces can be constructed from coarse wire
341:
is very large. As a consequence, 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 (10–100 MHz), they are generally either
679:
937:
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
310:
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.
577:, which also was the world's largest fully steerable telescope for 30 years until the Green Bank antenna was constructed. The third-largest fully steerable radio telescope is the 76-meter
2190:
631:
615:
604:
A more typical radio telescope has a single antenna of about 25 meters diameter. Dozens of radio telescopes of about this size are operated in radio observatories all over the world.
384:
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.
1251:
1848:
263:, 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
1740:
519:, though it suffered catastrophic collapse on 1 December 2020. Arecibo was one of the world's few radio telescope also capable of active (i.e., transmitting)
739:
Since 1965, humans have launched three space-based radio telescopes. The first one, KRT-10, was attached to Salyut 6 orbital space station in 1979. In 1997,
601:, at a diameter of 110 m (360 ft), is expected to become the world's largest fully steerable single-dish radio telescope when completed in 2028.
801:
161:
using an antenna built to study radio receiver noise. The first purpose-built radio telescope was a 9-meter parabolic dish constructed by radio amateur
102:
portion of the spectrum coming from astronomical objects. Unlike optical telescopes, radio telescopes can be used in the daytime as well as at night.
647:
1622:
895:. Interferometry does increase the total signal collected, but its primary purpose is to vastly increase the resolution through a process called
622:
488:
476:
1838:
1355:
1181:
1828:
663:
979:
686:
550:, which consists of a 576-meter circle of rectangular radio reflectors, each of which can be pointed towards a central conical receiver.
1763:
1398:
983:
1529:
19:
2468:
2219:
1942:
1779:
1098:
861:
574:
408:
1486:
Rohlfs, K., & Wilson, T. L. (2004). Tools of radio astronomy. Astronomy and astrophysics library. Berlin, Germany: Springer.
2180:
1902:
1382:
455:
275:, and by comparing his observations with optical astronomical maps, Jansky concluded that the radiation was coming from the
2156:
2050:
1154:
451:
769:
2148:
589:, England, completed in 1957. The fourth-largest fully steerable radio telescopes are six 70-meter dishes: three Russian
785:
1982:
1191:
1164:
1138:
1083:
872:
553:
The above stationary dishes are not fully "steerable"; they can only be aimed at points in an area of the sky near the
376:
The increasing use of radio frequencies for communication makes astronomical observations more and more difficult (see
1247:
557:, and cannot receive from sources near the horizon. The largest fully steerable dish radio telescope is the 100 meter
2619:
1818:
1640:
1583:
1501:
1215:
892:
2513:
2379:
1748:
1650:
702:
654:
566:
495:. The 500-meter-diameter (1,600 ft) dish with an area as large as 30 football fields is built into a natural
2254:
1872:
1577:
987:
900:
458:
in 5 different frequency bands, centered on 23 GHz, 33 GHz, 41 GHz, 61 GHz, and 94 GHz.
2235:
1972:
1808:
923:
2614:
1658:
1522:
722:
492:
423:", also known as the "21 centimeter line": 1,420.40575177 MHz, used by many radio telescopes including
271:
to come back to the same location in the sky. Thus Jansky suspected that the hiss originated outside of the
2604:
2422:
2100:
2000:
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135:
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1922:
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in 1937. The sky survey he performed is often considered the beginning of the field of radio astronomy.
2526:
1674:
1277:
1228:
831:
2609:
1962:
1882:
1599:
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consisting of 66 12-metre (39 ft), and 7-metre (23 ft) diameter radio telescopes designed to work at
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130:
and space probes. They may be used individually or linked together electronically in an array. Radio
75:
2503:
2172:
2140:
2040:
1716:
1604:
1515:
1302:
1088:
1007:
975:
582:
565:, United States, constructed in 2000. The largest fully steerable radio telescope in Europe is the
377:
334:
87:
986:
surveys of radio sources. An example of a large physically connected radio telescope array is the
2412:
2402:
1866:
1732:
1093:
931:
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512:
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One of the most notable developments came in 1946 with the introduction of the technique called
2124:
2010:
1014:
467:
193:
1372:
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2384:
2304:
1912:
1858:
1798:
1698:
1128:
946:
has 27 telescopes with 351 independent baselines at once, which achieves a resolution of 0.2
598:
1402:
2485:
2274:
2132:
1690:
1666:
971:
875:). All of the telescopes in the array are widely separated and are usually connected using
638:
558:
516:
381:
322:
8:
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2458:
2269:
2264:
2259:
2116:
2020:
1892:
1080:– distributed computing to search data tapes for primordial black holes, pulsars, and ETI
999:
943:
535:, giving use of a 270-meter diameter portion of the dish for any individual observation.
444:
343:
239:
158:
641:, Green Bank, West Virginia, US, the largest fully steerable radio telescope dish (2002)
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2438:
2407:
2354:
2314:
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1992:
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24:
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841:
670:
578:
500:
303:
276:
268:
218:
The first radio antenna used to identify an astronomical radio source was built by
368:
than 30 cm (above 1 GHz) range in size from 3 to 90 meters in diameter.
2374:
2319:
1538:
1108:
1040:
1026:
524:
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83:
79:
63:
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of a dish antenna is determined by the ratio of the diameter of the dish to the
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927:
865:
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338:
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189:
67:
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562:
543:
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420:
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280:
255:
919:
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The world's largest filled-aperture (i.e. full dish) radio telescope is the
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2294:
1567:
1489:
1255:
836:
532:
504:
403:
Some of the more notable frequency bands used by radio telescopes include:
352:
307:
272:
264:
447:
had several receivers that together covered the whole 1–10 GHz range.
34:
2473:
2364:
2359:
2289:
1051:, radio telescopes are able to "image" most astronomical objects such as
959:
951:
947:
428:
424:
291:
208:
162:
134:
are preferentially located far from major centers of population to avoid
131:
1303:"China Exclusive: China starts building world's largest radio telescope"
202:
1077:
413:
364:
318:
279:
and was strongest in the direction of the center of the galaxy, in the
260:
243:
139:
99:
78:
in the sky. Radio telescopes are the main observing instrument used in
71:
27:
as seen in 1969, when it was used to receive live televised video from
2478:
1706:
1332:
1103:
1036:
880:
539:
480:
251:
247:
223:
127:
28:
1186:(2 ed.). Springer Science & Business Media. pp. 8–10.
2339:
2191:
Special
Astrophysical Observatory of the Russian Academy of Science
2081:
808:
776:
752:
586:
1507:
1227:
Ley, Willy; Menzel, Donald H.; Richardson, Robert S. (June 1965).
226:, in 1932. Jansky was assigned the task of identifying sources of
1932:
1060:
47:
43:
1952:
1557:
1127:
Marr, Jonathan M.; Snell, Ronald L.; Kurtz, Stanley E. (2015).
1056:
1052:
1048:
1044:
748:
554:
547:
528:
235:
118:
114:
106:
302:
radio frequencies, discovering other radio sources. The rapid
2071:
995:
792:
744:
740:
726:
706:
590:
511:
The world's second largest filled-aperture telescope was the
496:
143:
126:
similar to those employed in tracking and communicating with
39:
1252:
Commonwealth
Scientific and Industrial Research Organisation
1553:
991:
966:
interferometer was also developed independently in 1946 by
908:
904:
570:
348:
326:
110:
2547:
538:
The largest individual radio telescope of any kind is the
1328:"China Finishes Building World's Largest Radio Telescope"
299:
188:
Full-size replica of the first radio telescope, Jansky's
146:, motor vehicles, and other man-made electronic devices.
1849:
Combined Array for
Research in Millimeter-wave Astronomy
1013:
The world's largest physically connected telescope, the
149:
Radio waves from space were first detected by engineer
1357:
China Begins
Operating World's Largest Radio Telescope
1130:
Fundamentals of Radio
Astronomy: Observational Methods
267:, the time it takes any "fixed" object located on the
94:
are the main observing instrument used in traditional
2524:
1031:
Many astronomical objects are not only observable in
1183:
The
Invisible Universe: The Story of Radio Astronomy
1159:. Encyclopædia Britannica, Inc. 2008. p. 1583.
907:
from the different telescopes on the principle that
1226:
294:, was one of the pioneers of what became known as
211:'s "dish" radio telescope, Wheaton, Illinois, 1937
1953:Multi-Element Radio Linked Interferometer Network
860:), arrays of one-dimensional antennas (e.g., the
16:Directional radio antenna used in radio astronomy
2596:
1496:. New York: Grosset & Dunlap. pp. 390–399.
1017:(SKA), is planned to start operations in 2025.
962:for interferometry and aperture synthesis. The
864:) or two-dimensional arrays of omnidirectional
623:Five-hundred-meter Aperture Spherical Telescope
489:Five-hundred-meter Aperture Spherical Telescope
1839:Canadian Hydrogen Intensity Mapping Experiment
1126:
1043:. Besides observing energetic objects such as
1523:
1829:Australian Square Kilometre Array Pathfinder
1020:
1623:500 meter Aperture Spherical Telescope
1364:
1220:
978:mapped the radio sky to produce the famous
832:Radio astronomy § Radio interferometry
734:
687:Goldstone Deep Space Communications Complex
483:(bottom) radio telescopes at the same scale
1530:
1516:
673:, Jodrell Bank Observatory, England (1957)
234:service. Jansky's antenna was an array of
1179:
1147:
172:
105:Since astronomical radio sources such as
90:emitted by astronomical objects, just as
1943:Molonglo Observatory Synthesis Telescope
1780:Warkworth Radio Astronomical Observatory
1173:
1099:Search for extraterrestrial intelligence
918:
893:Very Long Baseline Interferometry (VLBI)
862:Molonglo Observatory Synthesis Telescope
835:
625:(FAST), under construction, China (2016)
607:
575:Max Planck Institute for Radio Astronomy
466:
386:
317:
33:
18:
1370:
899:. This technique works by superposing (
848:formed of 27 parabolic dish telescopes.
819:
409:United States National Radio Quiet Zone
395:(or opacity) to various wavelengths of
2597:
1492:(1979). Isaac Asimov's Book of facts;
689:, Mojave Desert, California, US (1958)
685:The 70 meter DSS 14 "Mars" antenna at
2444:Cosmic microwave background radiation
2181:Pushchino Radio Astronomy Observatory
1903:Large Latin American Millimeter Array
1511:
657:, in Bad MĂĽnstereifel, Germany (1971)
456:cosmic microwave background radiation
2509:
2157:National Radio Astronomy Observatory
2051:Westerbork Synthesis Radio Telescope
1399:"Microwave Probing of the Invisible"
1353:
452:Wilkinson Microwave Anisotropy Probe
2149:Mullard Radio Astronomy Observatory
1537:
1354:Wong, Gillian (25 September 2016),
1120:
725:, Galenki, Russia, second of three
325:, a 326.5 MHz dipole array in
192:array of 1932, preserved at the US
13:
1983:Northern Extended Millimeter Array
1480:
1208:The Early Years of Radio Astronomy
1084:List of astronomical observatories
729:in the former Soviet Union, (1984)
709:in the former Soviet Union, (1978)
14:
2631:
1819:Australia Telescope Compact Array
1641:Caltech Submillimeter Observatory
1584:Very Long Baseline Interferometry
1245:
2582:
2570:
2558:
2546:
2534:
2508:
2499:
2498:
1059:, and even radio emissions from
800:
784:
768:
714:
694:
678:
662:
646:
630:
614:
567:Effelsberg 100-m Radio Telescope
433:1,406 MHz and 430 MHz
333:The range of frequencies in the
201:
181:
23:The 64-meter radio telescope at
1873:Giant Metrewave Radio Telescope
1741:UTR-2 decameter radio telescope
1463:
1445:
1431:
1417:
1391:
1347:
1156:Britannica Concise Encyclopedia
988:Giant Metrewave Radio Telescope
499:depression in the landscape in
50:. Consists of an array of 2040
42:low frequency radio telescope,
1973:Northern Cross Radio Telescope
1809:Atacama Large Millimeter Array
1320:
1295:
1270:
1239:
1210:. Cambridge University Press.
1200:
924:Atacama Large Millimeter Array
380:). Negotiations to defend the
371:
1:
1229:"The Observatory on the Moon"
1133:. CRC Press. pp. 21–24.
1114:
462:
196:in Green Bank, West Virginia.
2423:Gravitational-wave astronomy
2001:Primeval Structure Telescope
1471:"What are Radio Telescopes?"
911:that coincide with the same
523:of near-Earth objects (see:
491:(FAST) completed in 2016 by
391:Plot of Earth's atmospheric
136:electromagnetic interference
7:
2335:Christiaan Alexander Muller
2201:Vermilion River Observatory
2109:Algonquin Radio Observatory
1574:Astronomical interferometer
1377:. OUP Oxford. p. 139.
1066:
1004:Cosmic Microwave Background
854:astronomical interferometry
844:in Socorro, New Mexico, an
826:Astronomical interferometer
747:. The last one was sent by
573:, Germany, operated by the
290:An amateur radio operator,
224:Bell Telephone Laboratories
155:Bell Telephone Laboratories
124:parabolic ("dish") antennas
10:
2636:
1675:Large Millimeter Telescope
1453:"What is Radio Astronomy?"
1307:English.peopledaily.com.cn
1180:Verschuur, Gerrit (2007).
1024:
974:. In the early 1950s, the
950:at 3 cm wavelengths.
932:sub-millimeter wavelengths
829:
823:
355:. At shorter wavelengths
230:that might interfere with
76:astronomical radio sources
2494:
2431:
2393:
2247:
2212:
2099:
2064:
1963:Murchison Widefield Array
1883:Green Bank Interferometer
1791:
1707:RATAN-600 Radio Telescope
1613:
1598:
1590:Astronomical radio source
1545:
1374:A Dictionary of Astronomy
1021:Astronomical observations
998:. The largest array, the
705:, Crimea, first of three
440:: 1,420 to 1,666 MHz
397:electromagnetic radiation
357:parabolic "dish" antennas
2620:Astronomical instruments
2173:Onsala Space Observatory
2165:Nançay Radio Observatory
2141:Jodrell Bank Observatory
2041:Very Long Baseline Array
1717:Sardinia Radio Telescope
1231:. For Your Information.
1089:List of radio telescopes
1010:interferometer in 2004.
976:Cambridge Interferometer
735:Radiotelescopes in space
583:Jodrell Bank Observatory
531:by moving the suspended
427:in its discovery of the
335:electromagnetic spectrum
313:
88:electromagnetic spectrum
2403:Submillimetre astronomy
2015:Australia, South Africa
1867:Event Horizon Telescope
1206:Sullivan, W.T. (1984).
1094:List of telescope types
595:NASA Deep Space Network
513:Arecibo radio telescope
407:Every frequency in the
2125:Green Bank Observatory
2011:Square Kilometre Array
1442:vol.157, p. 158, 1946.
1428:vol.158, p. 339, 1946.
1233:Galaxy Science Fiction
1015:Square Kilometre Array
934:
849:
484:
400:
330:
194:Green Bank Observatory
173:Early radio telescopes
55:
31:
2418:High-energy astronomy
2305:Sebastian von Hoerner
1913:Long Wavelength Array
1859:European VLBI Network
1799:Allen Telescope Array
1699:Qitai Radio Telescope
1371:Ridpath, Ian (2012).
922:
846:interferometric array
839:
760:Space radiotelescopes
608:Gallery of big dishes
599:Qitai Radio Telescope
503:and cannot move; the
470:
416:: 608 to 614 MHz
390:
321:
37:
22:
2615:Astronomical imaging
2486:Solar radio emission
2275:Jocelyn Bell Burnell
2133:Haystack Observatory
1667:Green Bank Telescope
1651:Effelsberg Telescope
972:University of Sydney
820:Radio interferometry
639:Green Bank Telescope
559:Green Bank Telescope
517:Arecibo, Puerto Rico
382:frequency allocation
323:Ooty radio telescope
304:development of radar
242:designed to receive
165:in his back yard in
82:, which studies the
2605:American inventions
2459:Pulsar timing array
2265:Edward George Bowen
2255:Elizabeth Alexander
2117:Arecibo Observatory
2021:Submillimeter Array
1923:Low-Frequency Array
1893:Korean VLBI Network
1759:Southern Hemisphere
1670:(West Virginia, US)
1248:"The Dish turns 45"
1235:. pp. 132–150.
1000:Low-Frequency Array
944:Socorro, New Mexico
887:, or other type of
593:, and three in the
445:Arecibo Observatory
344:directional antenna
246:radio signals at a
222:, an engineer with
159:Holmdel, New Jersey
2439:Aperture synthesis
2408:Infrared astronomy
2345:Joseph Lade Pawsey
2315:Kenneth Kellermann
2285:Nan Dieter-Conklin
1993:One-Mile Telescope
1772:Parkes Observatory
1405:on August 31, 2007
1258:on August 24, 2008
1073:Aperture synthesis
956:group in Cambridge
935:
897:aperture synthesis
858:One-Mile Telescope
850:
485:
471:Comparison of the
401:
361:angular resolution
337:that makes up the
331:
138:(EMI) from radio,
98:which studies the
92:optical telescopes
56:
32:
25:Parkes Observatory
2522:
2521:
2464:Radio propagation
2413:Optical astronomy
2310:Karl Guthe Jansky
2120:(Puerto Rico, US)
2095:
2094:
1887:West Virginia, US
1636:(Puerto Rico, US)
1633:Arecibo Telescope
1384:978-0-19-960905-5
1041:radio wavelengths
889:transmission line
775:KRT-10 dish of a
743:sent the second,
359:predominate. The
220:Karl Guthe Jansky
167:Wheaton, Illinois
151:Karl Guthe Jansky
96:optical astronomy
62:is a specialized
2627:
2610:Radio telescopes
2587:
2586:
2585:
2575:
2574:
2573:
2563:
2562:
2561:
2551:
2550:
2539:
2538:
2537:
2530:
2512:
2511:
2502:
2501:
2479:HD 164595 signal
2454:Odd radio circle
2432:Related articles
2350:Ruby Payne-Scott
2280:Arthur Covington
2270:Ronald Bracewell
2240:
2232:
2224:
2205:
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2186:
2177:
2169:
2161:
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2145:
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2129:
2121:
2113:
2087:
2077:
2056:
2046:
2036:
2031:Very Large Array
2026:
2016:
2006:
1997:
1988:
1978:
1968:
1958:
1948:
1938:
1928:
1918:
1908:
1907:Argentina/Brazil
1898:
1888:
1878:
1863:
1854:
1844:
1834:
1824:
1814:
1804:
1784:
1776:
1768:
1760:
1753:
1749:Yevpatoria RT-70
1745:
1737:
1729:
1721:
1712:
1703:
1695:
1687:
1683:Lovell Telescope
1679:
1671:
1663:
1655:
1646:
1637:
1628:
1611:
1610:
1600:Radio telescopes
1532:
1525:
1518:
1509:
1508:
1475:
1474:
1467:
1461:
1460:
1449:
1443:
1435:
1429:
1421:
1415:
1414:
1412:
1410:
1401:. Archived from
1395:
1389:
1388:
1368:
1362:
1361:
1351:
1345:
1344:
1342:
1341:
1324:
1318:
1317:
1315:
1314:
1299:
1293:
1292:
1290:
1289:
1278:"Microstructure"
1274:
1268:
1267:
1265:
1263:
1254:. Archived from
1243:
1237:
1236:
1224:
1218:
1204:
1198:
1197:
1177:
1171:
1170:
1151:
1145:
1144:
1124:
970:'s group at the
940:Very Large Array
842:Very Large Array
804:
788:
772:
718:
703:Yevpatoria RT-70
698:
682:
666:
650:
634:
618:
579:Lovell Telescope
501:Guizhou province
277:Milky Way Galaxy
269:celestial sphere
205:
185:
2635:
2634:
2630:
2629:
2628:
2626:
2625:
2624:
2595:
2594:
2593:
2583:
2581:
2571:
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2559:
2557:
2545:
2535:
2533:
2525:
2523:
2518:
2490:
2427:
2395:
2389:
2375:Gart Westerhout
2243:
2238:
2230:
2222:
2208:
2203:
2194:
2184:
2183:(PRAO ASC LPI,
2175:
2167:
2159:
2151:
2143:
2135:
2127:
2119:
2111:
2091:
2085:
2075:
2060:
2054:
2044:
2034:
2024:
2014:
2004:
1995:
1986:
1976:
1966:
1956:
1946:
1936:
1926:
1916:
1906:
1896:
1886:
1876:
1861:
1852:
1842:
1832:
1822:
1812:
1802:
1792:Interferometers
1787:
1782:
1774:
1766:
1758:
1751:
1743:
1735:
1733:Usuda Telescope
1727:
1719:
1710:
1701:
1693:
1685:
1677:
1669:
1661:
1653:
1644:
1635:
1626:
1615:
1602:
1594:
1564:Radio telescope
1541:
1539:Radio astronomy
1536:
1483:
1481:Further reading
1478:
1469:
1468:
1464:
1451:
1450:
1446:
1436:
1432:
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1205:
1201:
1194:
1178:
1174:
1167:
1153:
1152:
1148:
1141:
1125:
1121:
1117:
1109:Radar telescope
1069:
1029:
1027:Radio astronomy
1023:
834:
828:
822:
817:
816:
815:
812:
805:
796:
789:
780:
773:
762:
761:
751:in 2011 called
737:
730:
719:
710:
699:
690:
683:
674:
667:
658:
651:
642:
635:
626:
619:
610:
525:radar astronomy
465:
374:
316:
296:radio astronomy
216:
215:
214:
213:
212:
206:
198:
197:
186:
175:
86:portion of the
84:radio frequency
80:radio astronomy
70:used to detect
60:radio telescope
17:
12:
11:
5:
2633:
2623:
2622:
2617:
2612:
2607:
2592:
2591:
2579:
2567:
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2491:
2489:
2488:
2483:
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2481:
2476:
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2461:
2456:
2451:
2449:Interferometry
2446:
2441:
2435:
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2429:
2428:
2426:
2425:
2420:
2415:
2410:
2405:
2399:
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2387:
2382:
2377:
2372:
2367:
2362:
2357:
2352:
2347:
2342:
2337:
2332:
2330:Bernard Lovell
2327:
2322:
2317:
2312:
2307:
2302:
2297:
2292:
2287:
2282:
2277:
2272:
2267:
2262:
2260:John G. Bolton
2257:
2251:
2249:
2245:
2244:
2242:
2241:
2233:
2228:ESA New Norcia
2225:
2216:
2214:
2210:
2209:
2207:
2206:
2198:
2188:
2178:
2170:
2162:
2154:
2146:
2138:
2130:
2122:
2114:
2105:
2103:
2097:
2096:
2093:
2092:
2090:
2089:
2079:
2068:
2066:
2062:
2061:
2059:
2058:
2048:
2038:
2035:New Mexico, US
2028:
2018:
2008:
1998:
1990:
1980:
1970:
1960:
1950:
1940:
1930:
1920:
1917:New Mexico, US
1910:
1900:
1890:
1880:
1870:
1864:
1856:
1853:California, US
1846:
1836:
1826:
1816:
1806:
1803:California, US
1795:
1793:
1789:
1788:
1786:
1785:
1777:
1769:
1767:(South Africa)
1761:
1755:
1754:
1746:
1738:
1730:
1722:
1714:
1704:
1696:
1691:Ooty Telescope
1688:
1680:
1672:
1664:
1656:
1648:
1638:
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1596:
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1534:
1527:
1520:
1512:
1506:
1505:
1487:
1482:
1479:
1477:
1476:
1462:
1457:Public Website
1444:
1430:
1416:
1390:
1383:
1363:
1346:
1319:
1294:
1269:
1238:
1219:
1199:
1193:978-0387683607
1192:
1172:
1166:978-1593394929
1165:
1146:
1140:978-1498770194
1139:
1118:
1116:
1113:
1112:
1111:
1106:
1101:
1096:
1091:
1086:
1081:
1075:
1068:
1065:
1035:but also emit
1025:Main article:
1022:
1019:
964:Lloyd's mirror
928:Atacama desert
824:Main article:
821:
818:
814:
813:
806:
799:
797:
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783:
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732:
731:
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700:
693:
691:
684:
677:
675:
668:
661:
659:
653:The 100 meter
652:
645:
643:
637:The 100 meter
636:
629:
627:
621:The 500 meter
620:
613:
609:
606:
597:. The planned
464:
461:
460:
459:
448:
441:
434:
431:
417:
411:
373:
370:
339:radio spectrum
315:
312:
232:radiotelephone
207:
200:
199:
187:
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176:
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171:
68:radio receiver
15:
9:
6:
4:
3:
2:
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2401:
2400:
2398:
2392:
2386:
2385:Robert Wilson
2383:
2381:
2378:
2376:
2373:
2371:
2370:Govind Swarup
2368:
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2341:
2338:
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2328:
2326:
2325:John D. Kraus
2323:
2321:
2320:Frank J. Kerr
2318:
2316:
2313:
2311:
2308:
2306:
2303:
2301:
2300:Antony Hewish
2298:
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2139:
2134:
2131:
2126:
2123:
2118:
2115:
2110:
2107:
2106:
2104:
2102:
2101:Observatories
2098:
2083:
2080:
2073:
2070:
2069:
2067:
2063:
2052:
2049:
2042:
2039:
2032:
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2022:
2019:
2012:
2009:
2002:
1999:
1994:
1991:
1984:
1981:
1974:
1971:
1964:
1961:
1954:
1951:
1944:
1941:
1934:
1931:
1924:
1921:
1914:
1911:
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1700:
1697:
1692:
1689:
1684:
1681:
1676:
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1668:
1665:
1660:
1659:Galenki RT-70
1657:
1652:
1649:
1642:
1639:
1634:
1631:
1624:
1621:
1620:
1618:
1612:
1609:
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1514:
1513:
1510:
1503:
1502:0-8038-9347-7
1499:
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1283:
1279:
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1253:
1249:
1242:
1234:
1230:
1223:
1217:
1216:0-521-25485-X
1213:
1209:
1203:
1195:
1189:
1185:
1184:
1176:
1168:
1162:
1158:
1157:
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1123:
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1110:
1107:
1105:
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1097:
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1090:
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1076:
1074:
1071:
1070:
1064:
1062:
1058:
1054:
1050:
1046:
1042:
1038:
1034:
1033:visible light
1028:
1018:
1016:
1011:
1009:
1005:
1001:
997:
993:
990:, located in
989:
985:
981:
977:
973:
969:
968:Joseph Pawsey
965:
961:
957:
953:
949:
945:
941:
933:
929:
925:
921:
917:
914:
910:
906:
903:) the signal
902:
898:
894:
890:
886:
885:optical fiber
882:
878:
877:coaxial cable
874:
871:
870:Tony Hewish's
867:
863:
859:
855:
847:
843:
838:
833:
827:
810:
803:
798:
794:
787:
782:
778:
771:
766:
765:
756:
754:
750:
746:
742:
728:
724:
723:Galenki RT-70
721:The 70 meter
717:
712:
708:
704:
701:The 70 meter
697:
692:
688:
681:
676:
672:
669:The 76 meter
665:
660:
656:
649:
644:
640:
633:
628:
624:
617:
612:
611:
605:
602:
600:
596:
592:
588:
584:
580:
576:
572:
568:
564:
563:West Virginia
560:
556:
551:
549:
545:
544:Nizhny Arkhyz
542:located near
541:
536:
534:
530:
526:
522:
521:radar imaging
518:
514:
509:
506:
502:
498:
494:
490:
482:
479:(middle) and
478:
474:
469:
457:
453:
449:
446:
442:
439:
435:
432:
430:
426:
422:
421:Hydrogen line
418:
415:
412:
410:
406:
405:
404:
398:
394:
393:transmittance
389:
385:
383:
379:
378:Open spectrum
369:
366:
362:
358:
354:
350:
345:
340:
336:
328:
324:
320:
311:
309:
305:
301:
297:
293:
288:
286:
282:
281:constellation
278:
274:
270:
266:
262:
257:
253:
249:
245:
241:
237:
233:
229:
225:
221:
210:
204:
195:
191:
184:
170:
168:
164:
160:
156:
152:
147:
145:
141:
137:
133:
132:observatories
129:
125:
120:
116:
112:
108:
103:
101:
97:
93:
89:
85:
81:
77:
73:
69:
65:
61:
53:
49:
45:
41:
36:
30:
26:
21:
2589:Solar System
2394:Astronomy by
2355:Arno Penzias
2295:Cyril Hazard
1937:South Africa
1728:(Uzbekistan)
1568:Radio window
1563:
1494:Sky Watchers
1493:
1465:
1456:
1447:
1437:
1433:
1423:
1419:
1407:. Retrieved
1403:the original
1393:
1373:
1366:
1356:
1349:
1338:. Retrieved
1336:. 2016-07-06
1331:
1322:
1311:. Retrieved
1309:. 2008-12-26
1306:
1297:
1286:. Retrieved
1284:. 1996-02-05
1282:Jb.man.ac.uk
1281:
1272:
1260:. Retrieved
1256:the original
1241:
1232:
1222:
1207:
1202:
1182:
1175:
1155:
1149:
1129:
1122:
1030:
1012:
936:
873:Pulsar Array
851:
738:
603:
552:
537:
533:feed antenna
510:
505:feed antenna
486:
402:
375:
353:chicken wire
332:
308:World War II
289:
273:Solar System
265:sidereal day
217:
148:
104:
59:
57:
2577:Outer space
2565:Spaceflight
2474:Wow! signal
2365:Martin Ryle
2360:Grote Reber
2290:Frank Drake
2231:(Australia)
2065:Space-based
2055:Netherlands
1927:Netherlands
1897:South Korea
1775:(Australia)
1725:Suffa RT-70
1262:October 16,
1006:, like the
960:Nobel Prize
958:obtained a
952:Martin Ryle
948:arc seconds
942:(VLA) near
901:interfering
811:dish (left)
515:located in
454:mapped the
429:Wow! signal
425:The Big Ear
372:Frequencies
292:Grote Reber
285:Sagittarius
163:Grote Reber
153:in 1932 at
72:radio waves
52:cage dipole
38:Antenna of
2599:Categories
2396:EM methods
1616:telescopes
1614:Individual
1490:Asimov, I.
1360:, ABC News
1340:2016-07-06
1313:2016-02-24
1288:2016-02-24
1115:References
1078:Astropulse
830:See also:
807:Assembled
779:on a stamp
655:Effelsberg
463:Big dishes
414:Channel 37
365:wavelength
261:shot noise
244:short wave
240:reflectors
140:television
128:satellites
100:light wave
54:elements.
2541:Astronomy
2380:Paul Wild
2213:Multi-use
2193:(SAORAS,
1967:Australia
1955:(MERLIN,
1947:Australia
1833:Australia
1823:Australia
1752:(Ukraine)
1744:(Ukraine)
1654:(Germany)
1333:Space.com
1104:Telescope
1037:radiation
881:waveguide
791:Japanese
540:RATAN-600
481:RATAN-600
438:Waterhole
300:very high
248:frequency
29:Apollo 11
2504:Category
2340:Jan Oort
2239:(Canada)
2223:(Canada)
2176:(Sweden)
2168:(France)
2112:(Canada)
2082:Spektr-R
1925:(LOFAR,
1905:(LLAMA,
1862:(Europe)
1851:(CARMA,
1841:(CHIME,
1831:(ASKAP,
1678:(Mexico)
1662:(Russia)
1546:Concepts
1409:June 13,
1067:See also
1053:galaxies
809:Spektr-R
777:Salyut-6
753:Spektr-R
587:Cheshire
351:such as
329:, India
250:of 20.5
119:galaxies
46:region,
2527:Portals
2514:Commons
2053:(WSRT,
2043:(VLBA,
2003:(PaST,
1945:(MOST,
1933:MeerKAT
1875:(GMRT,
1821:(ATCA,
1811:(ALMA,
1764:HartRAO
1736:(Japan)
1720:(Italy)
1702:(China)
1694:(India)
1625:(FAST,
1578:History
1552:Units (
1246:CSIRO.
1061:planets
1057:nebulae
1049:quasars
1045:pulsars
926:in the
868:(e.g.,
866:dipoles
475:(top),
473:Arecibo
306:during
236:dipoles
115:nebulas
107:planets
64:antenna
48:Ukraine
44:Kharkiv
2248:People
2195:Russia
2185:Russia
2086:Russia
2033:(VLA,
2023:(SMA,
2013:(SKA,
1987:France
1965:(MWA,
1915:(LWA,
1895:(KVN,
1885:(GBI,
1843:Canada
1801:(ATA,
1711:Russia
1643:(CSO,
1586:(VLBI)
1558:jansky
1500:
1439:Nature
1425:Nature
1381:
1214:
1190:
1163:
1137:
749:Russia
671:Lovell
555:zenith
548:Russia
529:zenith
256:analog
228:static
190:dipole
2553:Stars
2076:Japan
2072:HALCA
2005:China
1977:Italy
1877:India
1869:(EHT)
1813:Chile
1627:China
996:India
913:phase
909:waves
905:waves
793:HALCA
745:HALCA
741:Japan
727:RT-70
707:RT-70
591:RT-70
569:near
497:karst
493:China
419:The "
314:Types
209:Reber
144:radar
111:stars
74:from
40:UTR-2
2469:SETI
2236:PARL
2220:DRAO
2204:(US)
2160:(US)
2152:(UK)
2144:(UK)
2136:(US)
2128:(US)
1996:(UK)
1783:(NZ)
1686:(UK)
1605:List
1556:and
1554:watt
1498:ISBN
1411:2007
1379:ISBN
1264:2008
1212:ISBN
1188:ISBN
1161:ISBN
1135:ISBN
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