727:
707:
31:
813:
479:
797:
399:
691:
659:
627:
1013:(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
194:
46:
931:
848:
214:
675:
2510:
330:
265:(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
2570:
2594:
2520:
2546:
2582:
2558:
643:
726:
781:
519:
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.
378:
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
518:
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.
926:
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.
309:. 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
538:); 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
902:. 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
706:
132:
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
867:, 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
269:
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
357:
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
690:
352:
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
2200:
948:
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
321:
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.
626:
1262:
642:
588:, 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
1858:
1750:
615:
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.
812:
395:
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.
30:
1632:
633:
499:
487:
1848:
658:
274:, 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
530:, 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)
1838:
750:
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,
990:
697:
612:, 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.
1773:
994:
172:
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
674:
113:
portion of the spectrum coming from astronomical objects. Unlike optical telescopes, radio telescopes can be used in the daytime as well as at night.
1539:
2478:
2229:
1952:
1789:
1109:
872:
585:
906:. Interferometry does increase the total signal collected, but its primary purpose is to vastly increase the resolution through a process called
419:
2190:
1912:
1393:
1366:
1192:
466:
796:
2166:
2060:
462:
780:
561:, which consists of a 576-meter circle of rectangular radio reflectors, each of which can be pointed towards a central conical receiver.
2158:
1409:
1992:
1202:
1175:
1149:
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883:
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1828:
1650:
1593:
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903:
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713:
665:
577:
2264:
1882:
998:
911:
2245:
1982:
1818:
934:
286:, and by comparing his observations with optical astronomical maps, Jansky concluded that the radiation was coming from the
1165:
2624:
1668:
1532:
733:
503:
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600:, England, completed in 1957. The fourth-largest fully steerable radio telescopes are six 70-meter dishes: three Russian
2614:
2432:
2110:
2010:
966:
146:
1497:
Rohlfs, K., & Wilson, T. L. (2004). Tools of radio astronomy. Astronomy and astrophysics library. Berlin: Springer.
564:
The above stationary dishes are not fully "steerable"; they can only be aimed at points in an area of the sky near the
387:
The increasing use of radio frequencies for communication makes astronomical observations more and more difficult (see
2453:
2344:
2210:
2118:
1932:
1734:
1587:
1583:
1258:
1014:
864:
836:
568:, and cannot receive from sources near the horizon. The largest fully steerable dish radio telescope is the 100 meter
295:
165:
2174:
478:
2523:
1684:
506:. The 500-meter-diameter (1,600 ft) dish with an area as large as 30 football fields is built into a natural
2619:
1972:
1892:
1609:
1599:
407:
86:
469:
in 5 different frequency bands, centered on 23 GHz, 33 GHz, 41 GHz, 61 GHz, and 94 GHz.
2513:
2182:
2150:
2050:
1726:
1614:
1525:
1099:
1018:
986:
593:
345:
98:
2422:
2412:
1876:
1742:
1104:
942:
605:
523:
434:", also known as the "21 centimeter line": 1,420.40575177 MHz, used by many radio telescopes including
282:
to come back to the same location in the sky. Thus Jansky suspected that the hiss originated outside of the
1338:
2134:
2020:
1025:
204:
2427:
2394:
2314:
1922:
1868:
1808:
1708:
609:
398:
180:
in 1937. The sky survey he performed is often considered the beginning of the field of radio astronomy.
1288:
1239:
2495:
2284:
2142:
1700:
1676:
982:
941:
consisting of 66 12-metre (39 ft), and 7-metre (23 ft) diameter radio telescopes designed to work at
649:
569:
527:
392:
333:
141:
and space probes. They may be used individually or linked together electronically in an array. Radio
2598:
2468:
2279:
2274:
2269:
2126:
2030:
1902:
1313:
1010:
954:
576:, United States, constructed in 2000. The largest fully steerable radio telescope in Europe is the
455:
354:
250:
169:
997:
surveys of radio sources. An example of a large physically connected radio telescope array is the
2586:
2574:
2448:
2417:
2364:
2324:
2294:
2237:
2002:
1781:
1083:
907:
868:
371:
35:
863:
One of the most notable developments came in 1946 with the introduction of the technique called
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1508:
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1383:
1222:
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899:
483:
448:
367:
230:
193:
177:
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134:
106:
102:
1139:
957:
has 27 telescopes with 351 independent baselines at once, which achieves a resolution of 0.2
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2463:
2359:
2354:
2289:
2040:
1692:
1449:
1435:
1413:
1043:
950:
852:
681:
589:
511:
314:
287:
279:
930:
886:). All of the telescopes in the array are widely separated and are usually connected using
2384:
2329:
1548:
1119:
1051:
1037:
847:
842:
535:
306:
94:
90:
74:
1091:– distributed computing to search data tapes for primordial black holes, pulsars, and ETI
546:, giving use of a 270-meter diameter portion of the dish for any individual observation.
652:, Green Bank, West Virginia, US, the largest fully steerable radio telescope dish (2002)
45:
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1481:
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876:
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349:
242:
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200:
78:
62:
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266:
329:
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1500:
543:
515:
363:
318:
283:
275:
229:
The first radio antenna used to identify an astronomical radio source was built by
379:
than 30 cm (above 1 GHz) range in size from 3 to 90 meters in diameter.
2483:
2374:
2369:
2299:
1463:
970:
962:
958:
439:
435:
374:
of a dish antenna is determined by the ratio of the diameter of the dish to the
302:
219:
173:
142:
17:
1088:
424:
375:
271:
254:
150:
110:
82:
2488:
1716:
1343:
1114:
1047:
891:
550:
498:
The world's largest filled-aperture (i.e. full dish) radio telescope is the
491:
262:
258:
234:
138:
39:
1266:
414:
Some of the more notable frequency bands used by radio telescopes include:
458:
had several receivers that together covered the whole 1–10 GHz range.
2349:
2091:
1062:, radio telescopes are able to "image" most astronomical objects such as
819:
787:
763:
597:
145:
are preferentially located far from major centers of population to avoid
1314:"China Exclusive: China starts building world's largest radio telescope"
1942:
1071:
290:
and was strongest in the direction of the center of the galaxy, in the
89:
in the sky. Radio telescopes are the main observing instrument used in
58:
54:
38:
as seen in 1969, when it was used to receive live televised video from
1962:
1567:
1067:
1063:
1059:
1055:
759:
565:
558:
539:
246:
129:
125:
117:
1197:(2 ed.). Springer Science & Business Media. pp. 8–10.
2557:
2201:
Special
Astrophysical Observatory of the Russian Academy of Science
237:, in 1932. Jansky was assigned the task of identifying sources of
2081:
1517:
1238:
Ley, Willy; Menzel, Donald H.; Richardson, Robert S. (June 1965).
1006:
929:
846:
803:
755:
751:
737:
717:
601:
507:
397:
328:
154:
50:
44:
29:
1563:
1002:
919:
915:
581:
359:
337:
121:
1521:
1138:
Marr, Jonathan M.; Snell, Ronald L.; Kurtz, Stanley E. (2015).
313:
radio frequencies, discovering other radio sources. The rapid
310:
522:
The world's second largest filled-aperture telescope was the
137:
similar to those employed in tracking and communicating with
1263:
Commonwealth
Scientific and Industrial Research Organisation
977:
interferometer was also developed independently in 1946 by
549:
The largest individual radio telescope of any kind is the
1339:"China Finishes Building World's Largest Radio Telescope"
199:
Full-size replica of the first radio telescope, Jansky's
157:, motor vehicles, and other man-made electronic devices.
1859:
Combined Array for
Research in Millimeter-wave Astronomy
1024:
The world's largest physically connected telescope, the
160:
Radio waves from space were first detected by engineer
1368:
China Begins
Operating World's Largest Radio Telescope
1141:
Fundamentals of Radio
Astronomy: Observational Methods
278:, the time it takes any "fixed" object located on the
105:
are the main observing instrument used in traditional
2534:
1042:
Many astronomical objects are not only observable in
1194:
The
Invisible Universe: The Story of Radio Astronomy
1170:. Encyclopædia Britannica, Inc. 2008. p. 1583.
918:
from the different telescopes on the principle that
2441:
2403:
2257:
2222:
2109:
2074:
1801:
1623:
1608:
1555:
305:, was one of the pioneers of what became known as
222:'s "dish" radio telescope, Wheaton, Illinois, 1937
1963:Multi-Element Radio Linked Interferometer Network
871:), arrays of one-dimensional antennas (e.g., the
27:Directional radio antenna used in radio astronomy
1507:. New York: Grosset & Dunlap. pp. 390–399.
1028:(SKA), is planned to start operations in 2025.
973:for interferometry and aperture synthesis. The
875:) or two-dimensional arrays of omnidirectional
634:Five-hundred-meter Aperture Spherical Telescope
500:Five-hundred-meter Aperture Spherical Telescope
1849:Canadian Hydrogen Intensity Mapping Experiment
1054:. Besides observing energetic objects such as
1533:
8:
1839:Australian Square Kilometre Array Pathfinder
1633:500 meter Aperture Spherical Telescope
989:mapped the radio sky to produce the famous
843:Radio astronomy § Radio interferometry
698:Goldstone Deep Space Communications Complex
494:(bottom) radio telescopes at the same scale
1620:
1540:
1526:
1518:
684:, Jodrell Bank Observatory, England (1957)
245:service. Jansky's antenna was an array of
116:Since astronomical radio sources such as
101:emitted by astronomical objects, just as
1953:Molonglo Observatory Synthesis Telescope
1790:Warkworth Radio Astronomical Observatory
1110:Search for extraterrestrial intelligence
904:Very Long Baseline Interferometry (VLBI)
873:Molonglo Observatory Synthesis Telescope
636:(FAST), under construction, China (2016)
586:Max Planck Institute for Radio Astronomy
477:
2541:
1130:
910:. This technique works by superposing (
859:formed of 27 parabolic dish telescopes.
776:
622:
420:United States National Radio Quiet Zone
406:(or opacity) to various wavelengths of
1503:(1979). Isaac Asimov's Book of facts;
700:, Mojave Desert, California, US (1958)
696:The 70 meter DSS 14 "Mars" antenna at
2454:Cosmic microwave background radiation
2191:Pushchino Radio Astronomy Observatory
1913:Large Latin American Millimeter Array
668:, in Bad MĂĽnstereifel, Germany (1971)
467:cosmic microwave background radiation
7:
2519:
2167:National Radio Astronomy Observatory
2061:Westerbork Synthesis Radio Telescope
1410:"Microwave Probing of the Invisible"
463:Wilkinson Microwave Anisotropy Probe
2159:Mullard Radio Astronomy Observatory
1365:Wong, Gillian (25 September 2016),
736:, Galenki, Russia, second of three
336:, a 326.5 MHz dipole array in
203:array of 1932, preserved at the US
1993:Northern Extended Millimeter Array
1219:The Early Years of Radio Astronomy
1095:List of astronomical observatories
740:in the former Soviet Union, (1984)
720:in the former Soviet Union, (1978)
25:
1829:Australia Telescope Compact Array
1651:Caltech Submillimeter Observatory
1594:Very Long Baseline Interferometry
2592:
2580:
2568:
2556:
2544:
2518:
2509:
2508:
1070:, and even radio emissions from
811:
795:
779:
725:
705:
689:
673:
657:
641:
625:
578:Effelsberg 100-m Radio Telescope
444:1,406 MHz and 430 MHz
344:The range of frequencies in the
212:
192:
34:The 64-meter radio telescope at
1883:Giant Metrewave Radio Telescope
1751:UTR-2 decameter radio telescope
1167:Britannica Concise Encyclopedia
999:Giant Metrewave Radio Telescope
510:depression in the landscape in
61:. Consists of an array of 2040
53:low frequency radio telescope,
1983:Northern Cross Radio Telescope
1819:Atacama Large Millimeter Array
1221:. Cambridge University Press.
935:Atacama Large Millimeter Array
391:). Negotiations to defend the
1:
1240:"The Observatory on the Moon"
1144:. CRC Press. pp. 21–24.
207:in Green Bank, West Virginia.
2433:Gravitational-wave astronomy
2011:Primeval Structure Telescope
1482:"What are Radio Telescopes?"
922:that coincide with the same
534:of near-Earth objects (see:
502:(FAST) completed in 2016 by
402:Plot of Earth's atmospheric
147:electromagnetic interference
2345:Christiaan Alexander Muller
2211:Vermilion River Observatory
2119:Algonquin Radio Observatory
1584:Astronomical interferometer
1388:. OUP Oxford. p. 139.
1015:Cosmic Microwave Background
865:astronomical interferometry
855:in Socorro, New Mexico, an
837:Astronomical interferometer
758:. The last one was sent by
584:, Germany, operated by the
301:An amateur radio operator,
235:Bell Telephone Laboratories
166:Bell Telephone Laboratories
135:parabolic ("dish") antennas
2646:
1685:Large Millimeter Telescope
1464:"What is Radio Astronomy?"
1318:English.peopledaily.com.cn
1191:Verschuur, Gerrit (2007).
1035:
985:. In the early 1950s, the
961:at 3 cm wavelengths.
943:sub-millimeter wavelengths
840:
834:
366:. At shorter wavelengths
241:that might interfere with
87:astronomical radio sources
2504:
1973:Murchison Widefield Array
1893:Green Bank Interferometer
1717:RATAN-600 Radio Telescope
1600:Astronomical radio source
1385:A Dictionary of Astronomy
1032:Astronomical observations
1009:. The largest array, the
716:, Crimea, first of three
451:: 1,420 to 1,666 MHz
408:electromagnetic radiation
368:parabolic "dish" antennas
2630:Astronomical instruments
2183:Onsala Space Observatory
2175:Nançay Radio Observatory
2151:Jodrell Bank Observatory
2051:Very Long Baseline Array
1727:Sardinia Radio Telescope
1242:. For Your Information.
1100:List of radio telescopes
1021:interferometer in 2004.
987:Cambridge Interferometer
746:Radiotelescopes in space
594:Jodrell Bank Observatory
542:by moving the suspended
438:in its discovery of the
346:electromagnetic spectrum
99:electromagnetic spectrum
2413:Submillimetre astronomy
2025:Australia, South Africa
1877:Event Horizon Telescope
1217:Sullivan, W.T. (1984).
1105:List of telescope types
606:NASA Deep Space Network
524:Arecibo radio telescope
418:Every frequency in the
2135:Green Bank Observatory
2021:Square Kilometre Array
1244:Galaxy Science Fiction
1026:Square Kilometre Array
945:
860:
495:
411:
341:
205:Green Bank Observatory
184:Early radio telescopes
66:
42:
2428:High-energy astronomy
2315:Sebastian von Hoerner
1923:Long Wavelength Array
1869:European VLBI Network
1809:Allen Telescope Array
1709:Qitai Radio Telescope
1439:vol.158, p. 339, 1946
1382:Ridpath, Ian (2012).
933:
857:interferometric array
850:
771:Space radiotelescopes
619:Gallery of big dishes
610:Qitai Radio Telescope
514:and cannot move; the
481:
427:: 608 to 614 MHz
401:
332:
48:
33:
2625:Astronomical imaging
2496:Solar radio emission
2285:Jocelyn Bell Burnell
2143:Haystack Observatory
1677:Green Bank Telescope
1661:Effelsberg Telescope
1453:vol.157, p.158, 1946
983:University of Sydney
831:Radio interferometry
650:Green Bank Telescope
570:Green Bank Telescope
528:Arecibo, Puerto Rico
393:frequency allocation
334:Ooty radio telescope
315:development of radar
253:designed to receive
176:in his back yard in
93:, which studies the
2615:American inventions
2469:Pulsar timing array
2275:Edward George Bowen
2265:Elizabeth Alexander
2127:Arecibo Observatory
2031:Submillimeter Array
1933:Low-Frequency Array
1903:Korean VLBI Network
1769:Southern Hemisphere
1680:(West Virginia, US)
1259:"The Dish turns 45"
1246:. pp. 132–150.
1011:Low-Frequency Array
955:Socorro, New Mexico
898:, or other type of
604:, and three in the
456:Arecibo Observatory
355:directional antenna
257:radio signals at a
233:, an engineer with
170:Holmdel, New Jersey
2449:Aperture synthesis
2418:Infrared astronomy
2355:Joseph Lade Pawsey
2325:Kenneth Kellermann
2295:Nan Dieter-Conklin
2003:One-Mile Telescope
1782:Parkes Observatory
1416:on August 31, 2007
1269:on August 24, 2008
1084:Aperture synthesis
967:group in Cambridge
946:
908:aperture synthesis
869:One-Mile Telescope
861:
496:
482:Comparison of the
412:
372:angular resolution
348:that makes up the
342:
149:(EMI) from radio,
109:which studies the
103:optical telescopes
67:
43:
36:Parkes Observatory
2532:
2531:
2474:Radio propagation
2423:Optical astronomy
2320:Karl Guthe Jansky
2130:(Puerto Rico, US)
2105:
2104:
1897:West Virginia, US
1646:(Puerto Rico, US)
1643:Arecibo Telescope
1395:978-0-19-960905-5
1052:radio wavelengths
900:transmission line
786:KRT-10 dish of a
754:sent the second,
370:predominate. The
231:Karl Guthe Jansky
178:Wheaton, Illinois
162:Karl Guthe Jansky
107:optical astronomy
73:is a specialized
16:(Redirected from
2637:
2620:Radio telescopes
2597:
2596:
2595:
2585:
2584:
2583:
2573:
2572:
2571:
2561:
2560:
2549:
2548:
2547:
2540:
2522:
2521:
2512:
2511:
2489:HD 164595 signal
2464:Odd radio circle
2442:Related articles
2360:Ruby Payne-Scott
2290:Arthur Covington
2280:Ronald Bracewell
2250:
2242:
2234:
2215:
2206:
2196:
2187:
2179:
2171:
2163:
2155:
2147:
2139:
2131:
2123:
2097:
2087:
2066:
2056:
2046:
2041:Very Large Array
2036:
2026:
2016:
2007:
1998:
1988:
1978:
1968:
1958:
1948:
1938:
1928:
1918:
1917:Argentina/Brazil
1908:
1898:
1888:
1873:
1864:
1854:
1844:
1834:
1824:
1814:
1794:
1786:
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1770:
1763:
1759:Yevpatoria RT-70
1755:
1747:
1739:
1731:
1722:
1713:
1705:
1697:
1693:Lovell Telescope
1689:
1681:
1673:
1665:
1656:
1647:
1638:
1621:
1610:Radio telescopes
1542:
1535:
1528:
1519:
1486:
1485:
1478:
1472:
1471:
1460:
1454:
1446:
1440:
1432:
1426:
1425:
1423:
1421:
1412:. Archived from
1406:
1400:
1399:
1379:
1373:
1372:
1362:
1356:
1355:
1353:
1352:
1335:
1329:
1328:
1326:
1325:
1310:
1304:
1303:
1301:
1300:
1289:"Microstructure"
1285:
1279:
1278:
1276:
1274:
1265:. Archived from
1254:
1248:
1247:
1235:
1229:
1215:
1209:
1208:
1188:
1182:
1181:
1162:
1156:
1155:
1135:
981:'s group at the
951:Very Large Array
853:Very Large Array
815:
799:
783:
729:
714:Yevpatoria RT-70
709:
693:
677:
661:
645:
629:
590:Lovell Telescope
512:Guizhou province
288:Milky Way Galaxy
280:celestial sphere
216:
196:
21:
18:Radio telescopes
2645:
2644:
2640:
2639:
2638:
2636:
2635:
2634:
2605:
2604:
2603:
2593:
2591:
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2567:
2555:
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2535:
2533:
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2500:
2437:
2405:
2399:
2385:Gart Westerhout
2253:
2248:
2240:
2232:
2218:
2213:
2204:
2194:
2193:(PRAO ASC LPI,
2185:
2177:
2169:
2161:
2153:
2145:
2137:
2129:
2121:
2101:
2095:
2085:
2070:
2064:
2054:
2044:
2034:
2024:
2014:
2005:
1996:
1986:
1976:
1966:
1956:
1946:
1936:
1926:
1916:
1906:
1896:
1886:
1871:
1862:
1852:
1842:
1832:
1822:
1812:
1802:Interferometers
1797:
1792:
1784:
1776:
1768:
1761:
1753:
1745:
1743:Usuda Telescope
1737:
1729:
1720:
1711:
1703:
1695:
1687:
1679:
1671:
1663:
1654:
1645:
1636:
1625:
1612:
1604:
1574:Radio telescope
1551:
1549:Radio astronomy
1546:
1494:
1492:Further reading
1489:
1480:
1479:
1475:
1462:
1461:
1457:
1447:
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1190:
1189:
1185:
1178:
1164:
1163:
1159:
1152:
1137:
1136:
1132:
1128:
1120:Radar telescope
1080:
1040:
1038:Radio astronomy
1034:
845:
839:
833:
828:
827:
826:
823:
816:
807:
800:
791:
784:
773:
772:
762:in 2011 called
748:
741:
730:
721:
710:
701:
694:
685:
678:
669:
662:
653:
646:
637:
630:
621:
536:radar astronomy
476:
385:
327:
307:radio astronomy
227:
226:
225:
224:
223:
217:
209:
208:
197:
186:
97:portion of the
95:radio frequency
91:radio astronomy
81:used to detect
71:radio telescope
28:
23:
22:
15:
12:
11:
5:
2643:
2641:
2633:
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2622:
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2589:
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2501:
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2486:
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2471:
2466:
2461:
2459:Interferometry
2456:
2451:
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2439:
2438:
2436:
2435:
2430:
2425:
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2415:
2409:
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2392:
2387:
2382:
2377:
2372:
2367:
2362:
2357:
2352:
2347:
2342:
2340:Bernard Lovell
2337:
2332:
2327:
2322:
2317:
2312:
2307:
2302:
2297:
2292:
2287:
2282:
2277:
2272:
2270:John G. Bolton
2267:
2261:
2259:
2255:
2254:
2252:
2251:
2243:
2238:ESA New Norcia
2235:
2226:
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2216:
2208:
2198:
2188:
2180:
2172:
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2156:
2148:
2140:
2132:
2124:
2115:
2113:
2107:
2106:
2103:
2102:
2100:
2099:
2089:
2078:
2076:
2072:
2071:
2069:
2068:
2058:
2048:
2045:New Mexico, US
2038:
2028:
2018:
2008:
2000:
1990:
1980:
1970:
1960:
1950:
1940:
1930:
1927:New Mexico, US
1920:
1910:
1900:
1890:
1880:
1874:
1866:
1863:California, US
1856:
1846:
1836:
1826:
1816:
1813:California, US
1805:
1803:
1799:
1798:
1796:
1795:
1787:
1779:
1777:(South Africa)
1771:
1765:
1764:
1756:
1748:
1740:
1732:
1724:
1714:
1706:
1701:Ooty Telescope
1698:
1690:
1682:
1674:
1666:
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1629:
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1618:
1606:
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1537:
1530:
1522:
1516:
1515:
1498:
1493:
1490:
1488:
1487:
1473:
1468:Public Website
1455:
1441:
1427:
1401:
1394:
1374:
1357:
1330:
1305:
1280:
1249:
1230:
1210:
1204:978-0387683607
1203:
1183:
1177:978-1593394929
1176:
1157:
1151:978-1498770194
1150:
1129:
1127:
1124:
1123:
1122:
1117:
1112:
1107:
1102:
1097:
1092:
1086:
1079:
1076:
1046:but also emit
1036:Main article:
1033:
1030:
975:Lloyd's mirror
939:Atacama desert
835:Main article:
832:
829:
825:
824:
817:
810:
808:
801:
794:
792:
785:
778:
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769:
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747:
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743:
742:
731:
724:
722:
711:
704:
702:
695:
688:
686:
679:
672:
670:
664:The 100 meter
663:
656:
654:
648:The 100 meter
647:
640:
638:
632:The 500 meter
631:
624:
620:
617:
608:. The planned
475:
472:
471:
470:
459:
452:
445:
442:
428:
422:
384:
381:
350:radio spectrum
326:
323:
243:radiotelephone
218:
211:
210:
198:
191:
190:
189:
188:
187:
185:
182:
79:radio receiver
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
2642:
2631:
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2623:
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2426:
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2414:
2411:
2410:
2408:
2402:
2396:
2395:Robert Wilson
2393:
2391:
2388:
2386:
2383:
2381:
2380:Govind Swarup
2378:
2376:
2373:
2371:
2368:
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2363:
2361:
2358:
2356:
2353:
2351:
2348:
2346:
2343:
2341:
2338:
2336:
2335:John D. Kraus
2333:
2331:
2330:Frank J. Kerr
2328:
2326:
2323:
2321:
2318:
2316:
2313:
2311:
2310:Antony Hewish
2308:
2306:
2303:
2301:
2298:
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2144:
2141:
2136:
2133:
2128:
2125:
2120:
2117:
2116:
2114:
2112:
2111:Observatories
2108:
2093:
2090:
2083:
2080:
2079:
2077:
2073:
2062:
2059:
2052:
2049:
2042:
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2019:
2012:
2009:
2004:
2001:
1994:
1991:
1984:
1981:
1974:
1971:
1964:
1961:
1954:
1951:
1944:
1941:
1934:
1931:
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1911:
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1710:
1707:
1702:
1699:
1694:
1691:
1686:
1683:
1678:
1675:
1670:
1669:Galenki RT-70
1667:
1662:
1659:
1652:
1649:
1644:
1641:
1634:
1631:
1630:
1628:
1622:
1619:
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1514:
1513:0-8038-9347-7
1510:
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1268:
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1250:
1245:
1241:
1234:
1231:
1228:
1227:0-521-25485-X
1224:
1220:
1214:
1211:
1206:
1200:
1196:
1195:
1187:
1184:
1179:
1173:
1169:
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1125:
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1111:
1108:
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1103:
1101:
1098:
1096:
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1087:
1085:
1082:
1081:
1077:
1075:
1073:
1069:
1065:
1061:
1057:
1053:
1049:
1045:
1044:visible light
1039:
1031:
1029:
1027:
1022:
1020:
1016:
1012:
1008:
1004:
1001:, located in
1000:
996:
992:
988:
984:
980:
979:Joseph Pawsey
976:
972:
968:
964:
960:
956:
952:
944:
940:
936:
932:
928:
925:
921:
917:
914:) the signal
913:
909:
905:
901:
897:
896:optical fiber
893:
889:
888:coaxial cable
885:
882:
881:Tony Hewish's
878:
874:
870:
866:
858:
854:
849:
844:
838:
830:
821:
814:
809:
805:
798:
793:
789:
782:
777:
767:
765:
761:
757:
753:
745:
739:
735:
734:Galenki RT-70
732:The 70 meter
728:
723:
719:
715:
712:The 70 meter
708:
703:
699:
692:
687:
683:
680:The 76 meter
676:
671:
667:
660:
655:
651:
644:
639:
635:
628:
623:
618:
616:
613:
611:
607:
603:
599:
595:
591:
587:
583:
579:
575:
574:West Virginia
571:
567:
562:
560:
556:
555:Nizhny Arkhyz
553:located near
552:
547:
545:
541:
537:
533:
532:radar imaging
529:
525:
520:
517:
513:
509:
505:
501:
493:
490:(middle) and
489:
485:
480:
473:
468:
464:
460:
457:
453:
450:
446:
443:
441:
437:
433:
432:Hydrogen line
429:
426:
423:
421:
417:
416:
415:
409:
405:
404:transmittance
400:
396:
394:
390:
389:Open spectrum
382:
380:
377:
373:
369:
365:
361:
356:
351:
347:
339:
335:
331:
324:
322:
320:
316:
312:
308:
304:
299:
297:
293:
292:constellation
289:
285:
281:
277:
273:
268:
264:
260:
256:
252:
248:
244:
240:
236:
232:
221:
215:
206:
202:
195:
183:
181:
179:
175:
171:
167:
163:
158:
156:
152:
148:
144:
143:observatories
140:
136:
131:
127:
123:
119:
114:
112:
108:
104:
100:
96:
92:
88:
84:
80:
76:
72:
64:
60:
56:
52:
47:
41:
37:
32:
19:
2599:Solar System
2404:Astronomy by
2365:Arno Penzias
2305:Cyril Hazard
1947:South Africa
1738:(Uzbekistan)
1578:Radio window
1573:
1505:Sky Watchers
1504:
1476:
1467:
1458:
1448:
1444:
1434:
1430:
1418:. Retrieved
1414:the original
1404:
1384:
1377:
1367:
1360:
1349:. Retrieved
1347:. 2016-07-06
1342:
1333:
1322:. Retrieved
1320:. 2008-12-26
1317:
1308:
1297:. Retrieved
1295:. 1996-02-05
1293:Jb.man.ac.uk
1292:
1283:
1271:. Retrieved
1267:the original
1252:
1243:
1233:
1218:
1213:
1193:
1186:
1166:
1160:
1140:
1133:
1041:
1023:
947:
884:Pulsar Array
862:
749:
614:
563:
548:
544:feed antenna
521:
516:feed antenna
497:
413:
386:
364:chicken wire
343:
319:World War II
300:
284:Solar System
276:sidereal day
228:
159:
115:
70:
68:
2587:Outer space
2575:Spaceflight
2484:Wow! signal
2375:Martin Ryle
2370:Grote Reber
2300:Frank Drake
2241:(Australia)
2075:Space-based
2065:Netherlands
1937:Netherlands
1907:South Korea
1785:(Australia)
1735:Suffa RT-70
1273:October 16,
1017:, like the
971:Nobel Prize
969:obtained a
963:Martin Ryle
959:arc seconds
953:(VLA) near
912:interfering
822:dish (left)
526:located in
465:mapped the
440:Wow! signal
436:The Big Ear
383:Frequencies
303:Grote Reber
296:Sagittarius
174:Grote Reber
164:in 1932 at
83:radio waves
63:cage dipole
49:Antenna of
2609:Categories
2406:EM methods
1626:telescopes
1624:Individual
1501:Asimov, I.
1371:, ABC News
1351:2016-07-06
1324:2016-02-24
1299:2016-02-24
1126:References
1089:Astropulse
841:See also:
818:Assembled
790:on a stamp
666:Effelsberg
474:Big dishes
425:Channel 37
376:wavelength
272:shot noise
255:short wave
251:reflectors
151:television
139:satellites
111:light wave
65:elements.
2551:Astronomy
2390:Paul Wild
2223:Multi-use
2203:(SAORAS,
1977:Australia
1965:(MERLIN,
1957:Australia
1843:Australia
1833:Australia
1762:(Ukraine)
1754:(Ukraine)
1664:(Germany)
1344:Space.com
1115:Telescope
1048:radiation
892:waveguide
802:Japanese
551:RATAN-600
492:RATAN-600
449:Waterhole
311:very high
259:frequency
40:Apollo 11
2514:Category
2350:Jan Oort
2249:(Canada)
2233:(Canada)
2186:(Sweden)
2178:(France)
2122:(Canada)
2092:Spektr-R
1935:(LOFAR,
1915:(LLAMA,
1872:(Europe)
1861:(CARMA,
1851:(CHIME,
1841:(ASKAP,
1688:(Mexico)
1672:(Russia)
1556:Concepts
1420:June 13,
1078:See also
1064:galaxies
820:Spektr-R
788:Salyut-6
764:Spektr-R
598:Cheshire
362:such as
340:, India
261:of 20.5
130:galaxies
57:region,
2537:Portals
2524:Commons
2063:(WSRT,
2053:(VLBA,
2013:(PaST,
1955:(MOST,
1943:MeerKAT
1885:(GMRT,
1831:(ATCA,
1821:(ALMA,
1774:HartRAO
1746:(Japan)
1730:(Italy)
1712:(China)
1704:(India)
1635:(FAST,
1588:History
1562:Units (
1257:CSIRO.
1072:planets
1068:nebulae
1060:quasars
1056:pulsars
937:in the
879:(e.g.,
877:dipoles
486:(top),
484:Arecibo
317:during
247:dipoles
126:nebulas
118:planets
75:antenna
59:Ukraine
55:Kharkiv
2258:People
2205:Russia
2195:Russia
2096:Russia
2043:(VLA,
2033:(SMA,
2023:(SKA,
1997:France
1975:(MWA,
1925:(LWA,
1905:(KVN,
1895:(GBI,
1853:Canada
1811:(ATA,
1721:Russia
1653:(CSO,
1596:(VLBI)
1568:jansky
1511:
1450:Nature
1436:Nature
1392:
1225:
1201:
1174:
1148:
760:Russia
682:Lovell
566:zenith
559:Russia
540:zenith
267:analog
239:static
201:dipole
2563:Stars
2086:Japan
2082:HALCA
2015:China
1987:Italy
1887:India
1879:(EHT)
1823:Chile
1637:China
1007:India
924:phase
920:waves
916:waves
804:HALCA
756:HALCA
752:Japan
738:RT-70
718:RT-70
602:RT-70
580:near
508:karst
504:China
430:The "
325:Types
220:Reber
155:radar
122:stars
85:from
51:UTR-2
2479:SETI
2246:PARL
2230:DRAO
2214:(US)
2170:(US)
2162:(UK)
2154:(UK)
2146:(US)
2138:(US)
2006:(UK)
1793:(NZ)
1696:(UK)
1615:List
1566:and
1564:watt
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