 |
This is alist of radio telescopes – over one hundred – that are or have been used forradio astronomy. The list includes both singledishes andinterferometric arrays. The list is sorted by region, then by name; unnamed telescopes are in reverse size order at the end of the list.
The first radio telescope was invented in 1932, when Karl Jansky at Bell Telephone Laboratories observed radiation coming from the Milky Way.
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| AVN-Ghana | Kuntunse, Ghana | 3.8–6.4, 5, 6.7 GHz | 32-metre (104 foot) single dish, first of AfricanVLBI Network[1] |
| C-BASS South | Meerkat National Park, South Africa | 4.5–5.5 GHz | 7.6-metre (24.9 foot) dish with polarimeter back end[2] |
| HartRAO 26m | Hartebeesthoek Radio Astronomy Observatory,Johannesburg, South Africa | 1.66–23 GHz | 26 m dish.[3] |
| HartRAO XDM | Hartebeesthoek Radio Astronomy Observatory,Johannesburg, South Africa | 2.3–8.65 GHz | 15 mExperimental Demonstrator Model originally build as a technology demonstrator forMeerKAT[4] |
| Hydrogen Epoch of Reionization Array (HERA) | Meerkat National Park, South Africa | 50–200 MHz | In progress – currently nineteen 14 m reflectors with crossed dipole antennas as feed. |
| Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) | Meerkat National Park, South Africa | 400–800 MHz | In progress – currently eight 6 m dishes with dual-polarization dipole antennas as feed at HartRAO. |
| Indlebe | Durban University of Technology,Durban, South Africa | 1420 MHz | 5 meter (16 foot) parabolic reflector[5] |
| KAT-7 | Meerkat National Park, South Africa | 1200–1950 MHz | Seven, 12 meter (39 foot) dishes. |
| MeerKAT | Meerkat National Park, South Africa | 0.58–14.5 GHz | Sixty four, 13.5 m dishes. A pathfinder for theSquare Kilometre Array.[6] |
| Precision Array for Probing the Epoch of Reionization (PAPER) | Meerkat National Park, South Africa | 100–200 MHz | Now disassembled, PAPER at its maximum had 128 crossed dipole antennas,[7] making it theinterferometer with more elements than any other at that time. |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Degree Angular Scale Interferometer (DASI) | Amundsen–Scott South Pole Station | 26–36 GHz | 13-element interferometer measuring anisotropies in thecosmic microwave background.[8] |
| South Pole Telescope (SPT) | Amundsen–Scott South Pole Station | 95–350 GHz | 10-m microwave telescope making observations of clusters using theSunyaev-Zeldovich effect.[9] Also participates inEvent Horizon Telescope observations. |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Delingha 13.7 m | Delingha,Qinghai, China | 85–115 GHz | Dish diameter: 13.7 m. Site altitude: 3200 m. Operated byPurple Mountain Observatory. |
| Sheshan | Shanghai, China | 1660 MHz | 25 m. Operated by SHAO (Shanghai Astronomical Observatory) |
| Nanshan 25m | Ürümqi, China | 1.4–18 GHz | L/C/S/X band receivers. 70 km south to Ürümqi. Operated by XAO (Xinjiang Astronomical Observatory). |
| Primeval Structure Telescope (PaST) | Xinjiang, China | 50–200 MHz | PaST is planned to be an array of some ten-thousand log-periodic antennas spread over several square kilometers. Construction started in 2004. |
| Chinese Spectral Radio Heliograph (CSRH) | Inner Mongolia, China | 0.4–15 GHz | CSRH is an interferometer under construction in China. The CSRH will consist of 100 telescopes covering 0.4–15 GHz. 40 telescopes of 4.5 m cover 400 MHz – 2 GHz and 60 telescopes of 2 m cover 2–15 GHz. CSRH will be one of the world's largest and most advanced imaging spectroscopy instruments. CSRH will be used to study coronal mass ejections. All of the 4.5m telescopes are assembled and the 2m telescopes will be assembled by 2013.[10][11] |
| Miyun Synthesis Radio Telescope (MSRT) | Miyun, China | 232 MHz | Array of 28 9-meter dishes, completed in 1984. |
| Miyun 50m Radio Telescope | Miyun, China | 2–12 GHz | Built in 2005. |
| Kunming 40m Radio Telescope | Kunming, China | 2–12 GHz | Built in 2006. |
| Tianlai experiment cylinder pathfinder telescope | Hongliuxia, Balikun, Xinjiang, China | 500–1500 adjustable, currently 700–800 MHz | 3 cylinder reflectors, including a total of 96 dual-polarization receiver feeds, built in 2016 |
| Tianlai experiment dish pathfinder telescope | Hongliuxia, Balikun, Xinjiang, China | 500–1500 adjustable, currently 700–800 MHz | 16 dishes of 6m aperture, built in 2016 |
| Tian Ma 65m Radio Telescope | Shanghai, China | 1–50 GHz | Built in 2012.[12] Operated by SHAO (Shanghai Astronomical Observatory) |
| Giant Metrewave Radio Telescope (GMRT) | Pune,Maharashtra, India | 50–1420 MHz | Thirty 45 m wire dishes;[13] largest telescope at meterwavelengths. Operated by theNational Centre for Radio Astrophysics.[14] |
| Ooty Radio Telescope (ORT) | Ooty,Tamil Nadu, India | 326.5 MHz | Theradio telescope is a 530-metre (1,740 ft) long and 30-metre (98 ft) tall cylindricalparabolic antenna. It operates at a frequency of 326.5 MHz with a maximum bandwidth of 15 MHz at the front end. |
| Gauribidanur Radio Observatory | Gauribidanur, Karnataka, India | 40–150 MHz | Operated by (Indian Institute of Astrophysics). A Radioheliograph. |
| Nobeyama radio observatory | Nagano Prefecture, Japan | 17–115 GHz | A 45 m single-dish short-millimetre telescope, and six 10 m telescopes of the Nobeyama Millimetre Array (NMA), both operated by theNational Astronomical Observatory of Japan (NAOJ) |
| Siberian Solar Radio Telescope (SSRT) | Badary, Buryatia, Russia | 5.7 GHz | The SSRT is a crossed interferometer, consisting of two arrays of 128x128 parabolic antennas 2.5 meters in diameter each, spaced equidistantly at 4.9 meters and oriented in the E-W and N-S directions. The SSRT is a special-purpose solar radio telescope designed for studying solar activity in the microwave range (5.7 GHz).[15] |
| Badary Radio Astronomical Observatory | Badary, Buryatia, Russia | 1.4–22 GHz | 32 m RT-32 radio telescope, operating range 1.4–22 GHz.[16] |
| Galenki RT-70 radio telescope | Galenki (Ussuriysk), Russia | 5–300 GHz | RT-70, 70 m telescope, operating range 5–300 GHz |
| Suffa RT-70 radio telescope | Suffa plateau, Uzbekistan | 5–300 GHz | RT-70, the construction started in 1981 but was never completed. |
| Five hundred meter Aperture Spherical Telescope (FAST) | Guizhou, China | 70–3000 MHz | 500m radio telescope, the world's largest filled-aperture radio telescope, operating range 70–3000 MHz.[17] |
| Qitai Radio Telescope | Qitai County,Xinjiang, China | 300 MHz–117 GHz | Construction work started in 2012. Will be operated by XAO (Xinjiang Astronomical Observatory). |
| Thai National Radio Telescope | Chiang Mai, Thailand | 300 MHz–115 GHz | Construction work started in 2017. A 40m single-dish short-millimetre telescope,[18] operated by theNational Astronomical Research Institute of Thailand (NARIT).[19] |
| VERA | Japan | 6.7 GHz–43 GHz | A VLBI system with four 20-m telescopes in Japan (Mizusawa,Chichijima,Iriki,Ishigaki island)[20] operated by theNational Astronomical Observatory of Japan (NAOJ). |
| Daocheng Solar Radio Telescope | Sichuan province, China | 150 MHz–450 MHz | 313 parabolic antennas for detection ofcoronal mass ejection events. Operations started in 2023.[21] |
| Mingantu interplanetary scintillation telescope | Inner Mongolia, China | 327 MHz and 654 MHz[22] | interplanetary scintillation telescope, consists of three rotatable cylindrical antennas (140 metres by 40 metres each).[23] |
| Taeduk Radio Astronomy Observatory (TRAO) | Daejeon, Republic of Korea | 86–115 GHz | TRAO was established in October 1986 with the 13.7 meter Radio Telescope. It opened the new era of the millimeter-wave radio astronomy in Korea as one of the main facilities of Korea Astronomy and Space science Institute[24] (KASI). It is operated by Radio astronomy division in KASI.[25] |
| Korean VLBI Network (KVN) | Republic of Korea | 22/43/86/129 GHz | KVN consists of four 21-m radio telescopes located inSeoul,Ulsan,Jeju Island andPyeongchang (Constructing), Republic of Korea. They have an identical design and are equipped with a quasi-optical system that allows simultaneous observations at 22, 43, 86, and 129 GHz. Since August in 2013, KVN Ulsan have started to operate 6.7 GHz in single-dish and VLBI modes.[26] |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Australian Square Kilometre Array Pathfinder (ASKAP) | Murchison Radio-astronomy Observatory, Western Australia | 700–1800 MHz | ASKAP, the Australian Square Kilometre Array Pathfinder, is operated byCSIRO. It is made up of 36 identical antennas, each 12 metres in diameter, with a 30 sq degrees FoV at 1.4 GHz.[27] |
| Australia Telescope Compact Array (ATCA) | Paul Wild Observatory,Narrabri, New South Wales | 0.3–110 GHz | 6x22m dishaperture synthesis array, operated byCSIRO as part of the ATNF (Australia Telescope National Facility).[28] |
| Canberra Deep Space Communication Complex (CDSCC) | Tidbinbilla, Australian Capital Territory | 1x70 m dish, 3x34 m dishes, operated byCSIRO on behalf ofNASA.[29] | |
| Ceduna Radio Observatory | Ceduna, South Australia | 1.2–23 GHz | 30 m telescope, operated by theUniversity of Tasmania |
| Molonglo Observatory Synthesis Telescope (MOST) | Molonglo (nearCanberra, Australian Capital Territory) | 600–1200 MHz | Operated by the School of Physics at theUniversity of Sydney. East-west arm of the formerMolonglo Cross Telescope, approximately 1.6 km in length. Operates at 843 MHz. |
| Mopra Radio Telescope | Mopra Observatory, nearCoonabarabran, New South Wales | 0.3–100 GHz | 22 m dish, operated byCSIRO as part of the ATNF (Australia Telescope National Facility).[30] |
| Mount Pleasant Radio Telescope | Hobart, Tasmania | 1.2–23 GHz | 26 m telescope, operated by theUniversity of Tasmania |
| Murchison Widefield Array (MWA) | Murchison Radio-astronomy Observatory, Western Australia | 70–300 MHz | Fixed 256 array of 16-element dual-polarisation antennas covering 70–300 MHz with approximately 30° field-of-view using electronic beam-forming |
| Parkes Radio Telescope | Parkes Observatory, New South Wales | 64 m telescope (2nd largest movable dish in the Southern Hemisphere), operated byCSIRO as part of the ATNF (Australia Telescope National Facility).[31] |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Effelsberg 100-m Radio Telescope | Bad Münstereifel-Effelsberg nearBonn, Germany | 395 MHz – 95 GHz | 100 m fully steerable dish operated byMax Planck Institut für Radioastronomie, operates at 395 MHz to 95 GHz |
| Ukrainian T-shaped Radio telescope, second modification (UTR-2) | Volokhiv Yar,Kharkiv, Ukraine | 8–33 MHz | World's largest radio telescope atdecametre wavelengths (max. collective area 150,000 m2). |
| Giant Ukrainian Radio Telescope (GURT) | Volokhiv Yar,Kharkiv, Ukraine | 8–80 MHz | Low-frequency radio telescope of new generation. Construction is in progress, separate 25-element subarrays are used for observations of Sun, Jupiter, pulsars. |
| Lovell Telescope | Jodrell Bank Observatory,Cheshire, England | 0–2 GHz | 76 m dish |
| Yevpatoria RT-70 radio telescope | former soviet Center for deep space communications,Yevpatoria,Crimea | 5–300 GHz | RT-70, 70 m telescope, operating range 5–300 GHz |
| RATAN-600 | Zelenchukskaya, Russia | 0.61–30 GHz | 600 m dish, operates at 610 MHz to 30 GHz, world's largest diameter individual radio telescope |
| RT-64 (TNA-1500) | Kalyazin, Russia[32] | 5.86 GHz | 64 m fully steerable dish, up to 5.86 GHz |
| RT-64 (TNA-1500) | Medvezhji Ozera (Bear Lakes), Russia[32] | 5.86 GHz | 64 m fully steerable dish, up to 5.86 GHz |
| RT-22 | Pushchino, Russia | Four 22 m fully steerable radio telescopes. At the 1960s the centimeter and millimeter-wavelength RT-22s had a world record-breaking high angular resolution for individual radio telescopes. Operated by thePushchino Radio Astronomy Observatory. | |
| DKR-1000 | Pushchino, Russia | DKR-1000 is the world largest telescope operating in the meter wavelength range. A wide-band radio telescope instrument consists of two parabolic cylinders 1 km long and 40 m width. One cylinder extend from east to west and the 2nd from north to south. DKR-1000 has a high sensitivity and the telescope allows simultaneous observations at any wavelengths in the range from 2.5m to 10m. Operated by thePushchino Radio Astronomy Observatory.[33] | |
| BSA | Pushchino, Russia | BSA is a Large Phased Array comprising over 16,000 dipoles and covering an area of 7.2 hectares. The BSA has a world record sensitivity in the meter wavelength range. Operated by thePushchino Radio Astronomy Observatory.[33] | |
| Radioastronomical ObservatoryZelenchukskaya | Karachaevo-Cherkessiya, Russia | 1.4–22 GHz | 32m RT-32 radio telescope, operating range 1.4–22 GHz.[2][dead link] |
| Svetloe Radio Astronomical Observatory | Svetloe, Karelia, Russia | 1.4–22 GHz | 32m RT-32 radio telescope, operating range 1.4–22 GHz.[34] |
| RT-7.5 (Bauman's radio telescope) | Moscow Oblast, Russia | Two 7.75-meter diameter antennas (only one is working at the moment)[35] | |
| Yebes RT 40 m | Spanish National Observatory,Yebes,Guadalajara, Spain[36] | 40 m parabolic steerable telescope for mm and cm wavelengths | |
| Toruń RT4 32 m | Toruń Centre for Astronomy,Toruń, Poland | RT4 (32 m)parabolic antenna | |
| RT-32 | Ventspils International Radio Astronomy Center,Irbene, Latvia | 32-meter fully steerable parabolic, centimetre-wave range antenna RT-32[37] | |
| Northern Cross Radio Telescope | Medicina Radio Observatory,Medicina,Bologna, Italy[38] | 408 MHz | 32000 m2 interferometer, cylindrical-paraboloid steerable over NS., 408 MHz, Beam=3' |
| 32 m VLBI dish | Medicina Radio Observatory,Medicina,Bologna, Italy[38] | 1.4–43 GHz | 32 m, fully steerable dish, 1400 MHz...43 GHz |
| 32 m VLBI dish | Noto Radio Observatory,Noto, Italy,[38] | 0.3–86 GHz | 32 m, fully steerable dish, 300 MHz – 86 GHz. Operates both as part of astronomical and geodetic VLBI network and as a single dish. |
| MERLIN (Multi-Element Radio Linked Interferometer Network) | United Kingdom | 151 MHz – 24 GHz | Consists of the Cambridge 32 m atMullard Radio Astronomy Observatory,Darnhall,Defford, Tabley (also known asPickmere) andKnockin. Also includes theLovell andMark II telescopes atJodrell Bank. |
| EAARO – East Anglian Astrophysical Research Organisation | Cambridgeshire, England[39] | 0–11 GHz | A scientific and educational charitable company currently constructing a Radio Observatory and Ground Station in Cambridgeshire |
| TNA-400 | Center for deep space communications,Simferopol,Crimea | TNA-400 [ru], 32 m telescope | |
| IRAM – 30m | Pico Veleta, inGranada, Spain | 30m dish operated by the Institute for Millimetric Radio Astronomy (Institut de radioastronomie millimétrique, IRAM); works in the millimeter range (1mm to 3mm) both withsuperheterodyne andbolometric detectors. | |
| Mark II | Jodrell Bank Observatory,Cheshire, England | 0–24 GHz | 25 m dish |
| Stockert | Bad Münstereifel-Eschweiler nearBonn, Germany | 25 m dish operated byUniversity of Bonn andMax Planck Institut für Radioastronomie, closed in 1993, now owned by NRW-Stiftung,[40] reopened 2010 after restoration and operated by Förderverein Astropeiler Stockert[41] | |
| Toruń RT3 15 m | Toruń Centre for Astronomy,Toruń, Poland | RT3 (15 m) antenna. | |
| Westerbork Synthesis Radio Telescope (WSRT) | Westerbork, Netherlands | 2.8 km array of 14 25-meter dishes operated byASTRON | |
| 25 m telescope | Onsala Space Observatory,Onsala, Sweden | 25 m telescope | |
| Dwingeloo (CAMRAS) | Dwingeloo, Netherlands | 25 m steerable dish, formerly operated byASTRON, now operated by CAMRAS[42] | |
| 22 m telescope | Simeiz Observatory,Simeiz,Crimea | 22-m radio telescope for mm and cm radio waves. Located at the foot of mount Koshka (Cat) in Katsiveli (near Simeiz). Belongs to the Crimean Astrophysical Observatory, the Department of Radioastronomy. | |
| 20 m telescope | Onsala Space Observatory,Onsala, Sweden | 20 m telescope | |
| Pluton (complex) | Center for deep space communications,Yevpatoria,Crimea | 8 mirrors with diameter of 16 meters. Square is 1000 sq. meters. | |
| RT-16 | Ventspils International Radio Astronomy Center,Irbene, Latvia | 16-meter diameter antenna RT-16[37] | |
| KAIRA | Kilpisjärvi,Enontekiö, Finland | 30 m × 50 m, 768-element phased array and a 34 m diameter, 48-element phased array | |
| Metsähovi Radio Observatory | Kylmälä,Kirkkonummi, Finland | 2–150 GHz | 13.7 m dish, operates at 2 to 150 GHz, surface accuracy 0.1 mm (rms). |
| Ryle Telescope | Mullard Radio Astronomy Observatory,Cambridge, England | Eight 13 m dishes, and is currently used as one part of theArcminute Microkelvin Imager. | |
| Erciyes University Radio Observatory | Kayseri, Turkey | 12.8 m dish | |
| Wurzburg v2.0 LAB/OASU (Bordeaux Observatory radio telescope) | Floirac, Gironde, France | 1.4–1.7 GHz | 7.5 meter diameter antenna. Observable frequency range : 1.4–1.7 GHz. Bandwidth ≈9.2 MHz[43] |
| European VLBI Network (EVN) | Distributed across Europe with members in China, South Africa and the US | VLBI array operated bythe European Consortium for VLBI | |
| Plateau de Bure Interferometer | Plateau de Bure,Grenoble, France | Originally an array of 3 antennas, since 2005 has 6 antennas, operating at millimeter wavelengths, now part of NOEMA | |
| Northern Extended Millimeter Array (NOEMA) | Plateau de Bure,Grenoble, France | 12 antennas, operating at millimeter wavelengths (Operational: 2019). | |
| Nançay Radio Telescope (NRT) | Nançay, France | NRT website (fr) | |
| Nançay Decameter Array (DAM) | Nançay, France | 10–100 MHz | DAM website (fr) |
| Nançay Radio Heliographe (NRH) | Nançay, France | 150–450 MHz | NRH website (fr) |
| ALLBIN (Amateur Linked Long Baseline Interferometer Network) | Germany | A Small Network of Radio Telescopes and Radio Spectrographs doing Amateur Radio Astronomy at a Very High standard coordinated byThe European Radio Astronomy Club[44] Research and Development Telescope in Mannheim Germany. | |
| LOFAR (LOw Frequency ARray) | Netherlands, Germany, Great Britain, France, Sweden, Poland, Ireland; in future possibly other countries | 10–240 MHz | Low frequency array of dipole antennas at 1.25 to 30m wavelengths (10–240 MHz), with a strongly distributed signal processing system. The telescope beam is constructed in software from combinations of antenna signals. Operated byASTRON |
| São Gião radio telescope (SGRT) | São Gião, Portugal | 0.4–22 GHz | 9.3 m solid surface dish, operated by PARAC[45] |
| Arcminute Microkelvin Imager | Mullard Radio Astronomy Observatory,Cambridge, England | Small Array consists of 10 3.7-m parabolic antennas | |
| The European Radio Astronomy Club Telescope and Development Facility (ERAC Telescope) | Mannheim, Germany | From 14 kHz VLF up to 40 GHz[46] | |
| ERAC Phased Array | The European Radio Astronomy Club,Elsass, France | Phased array and Digital back end based on the SKA design | |
| ERAC Phased Array | The European Radio Astronomy Club,East Lothian, Scotland | Phased array and Digital back end based on the SKA design | |
| 64 m Sardinia Radio Telescope | San Basilio, Sardinia, Italy | Sardinia Radio Telescope. 64 m dish. | |
| ROT-54/2.6 | Mount Aragats, Armenia, nearYerevan | 1.5–300 GHz | Radio optical Telescope with 54 m Spherical Reflector Antenna and 2.6 m optical telescope on the same axis. One of the most sensitive and low noise antennas in the world. Operating during 1987–2010. Conserved from 2015. It is planned to revitalize it in 2020–2025 by the force of Armenian and International science-technical society. However a 2019 video report shows that the place has been abandoned and scavenged.[47] |
| Bayfordbury Observatory | Hertfordshire,UK | 1.4 GHz | 4.5 m single dish, and 115 m baseline 3 dish interferometer. Operated by theUniversity of Hertfordshire |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Algonquin 46m radio telescope | Algonquin Radio Observatory,Algonquin Park,Ontario, Canada | 46 metre fully steerable dish operated by Thoth Technology,[48] Canada's largest radio telescope. | |
| Allen Telescope Array | Hat Creek Radio Observatory,Hat Creek, California, US | 0.5–11.5 GHz | 42 6-mgregorian offset dishes using log periodic cooled feed covering 0.5–11.5 GHz. Operated by joint agreement betweenSRI International and theSETI Institute |
| ARO 12m Radio Telescope | Kitt Peak National Observatory,Tucson, Arizona, US | Previously operated by theNRAO, this telescope is currently operated by theUniversity of Arizona'sArizona Radio Observatory, part ofSteward Observatory. | |
| C-BASS North | Owens Valley Radio Observatory,Big Pine, California, US | 4.5–5.5 GHz | 6.1 metre dish with polarimeter back end.[2] This telescope was decommissioned in April 2015. |
| Canadian Hydrogen Intensity Mapping Experiment (CHIME) | Dominion Radio Astrophysical Observatory,Kaleden, British Columbia, Canada | 400–800 MHz | A novel drift scan telescope, which consists of four 100 × 20meter 5 m focal length cylinders, with an array of 256 dual-polarized radio receivers along the focus. Will map the21 cm line of neutral hydrogen over the cosmologicalredshift range of 0.8 to 2.5. Collected its first light in September 2017.[49] |
| CfA 1.2 m Millimeter-Wave Telescope | Center for Astrophysics | Harvard & Smithsonian,Cambridge, Massachusetts, US | 115 GHz | A small radio telescope which, along with a twin instrument in Chile, has been continuously mapping interstellarcarbon monoxide since the 1970s. |
| Combined Array for Research in Millimeter-wave Astronomy (CARMA) | Owens Valley Radio Observatory,Big Pine, California, US | 75–345 GHz | Heterogeneousinterferometer array composed of 6 10-m elements, 9 6-m elements, and 8 3.5-m elements covering frequencies ranging from 27 to 36 GHz, 80 to 115 GHz, and 215 to 265 GHz. Operated by joint agreements betweenRadio Astronomy LaboratoryUniversity of California, Berkeley,Caltech,University of Maryland, College Park,University of Illinois Urbana-Champaign, and theUniversity of Chicago. |
| Distributed Array Radio Telescope (DART) | https://erau-prescott-observatory.com/ Embry-Riddle Radio Observatory, Prescott AZ], US | 100–300 MHz | Array of three 16-element dual-polarization tiles with electronic beam-forming. Identical to the original MWA design |
| Dominion Radio Astrophysical Observatory | Kaleden, British Columbia, Canada | 408–1420 MHz | Synthesis telescope consists of seven 9-metre (30 ft)parabolic antennas, three of which are movable along a 600-metre rail line. |
| DSA-110 | Owens Valley Radio Observatory,Big Pine, California, US | 1280–1530 MHz | Array of 110 dishes of 5 meter diameter. Optimized for detecting and localizingfast radio bursts. |
| Deep Synoptic Array | Spring Valley, White Pine County,Nevada, US | 700–2000 MHz | Array of 1650 dishes of 6.15 meter diameter; main goal is an imaging sky survey. Currently under construction. |
| Five College Radio Astronomy Observatory (FCRAO) | Amherst, Massachusetts, US | Operated byUMass Amherst | |
| Goldstone Radio Telescope | Mojave Desert, California, US | One of the most sensitive radars in the world | |
| Green Bank Interferometer (GBI) | Green Bank, West Virginia, US | Three 26 meters (85 feet) radio telescopes formerly operated byNRAO, and now kept byGBO as a historic telescope. | |
| Green Bank Telescope (GBT) | Green Bank, West Virginia, US | 0.29–2.6 GHz; 2.95–7.8 GHz; 8–10 GHz; 12–15.4 GHz; 18–47 GHz; 67–100 GHz. | World's largest 100-metre (330 ft) fully steerable single-dish radio telescope |
| Green Bank 140 Foot Telescope (140foot) | Green Bank, West Virginia, US | 0.75–15.0 GHz (2–40 cm) | 43 m equatorial mount single-dish radio telescope. Currently awaiting its next mission.[50] |
| Green Bank 20m Telescope | Green Bank, West Virginia, US | 20m telescope, fully automated and accessed through theUniversity of North Carolina'sSkynet Robotic Telescope Network. | |
| Haystack Observatory | Westford, Massachusetts, US | 37 m radome-enclosed 90 GHz radar/radiotelescope; 9 m radar for space debris tracking, 46 m incoherent scatter radar, 26 m L-band deep space tracking radar, 18 m radiotelescope used for geodesy. Operated by theMassachusetts Institute of Technology | |
| Heinrich Hertz Submillimeter Telescope (SMT) | Mount Graham,Arizona, US | 10-meter radio telescope operated by theUniversity of Arizona'sArizona Radio Observatory, part ofSteward Observatory. | |
| Hydrogen Epoch of Reionization Array (HERA) | Embry-Riddle Radio Observatory, Prescott AZ, US | 100–200 MHz | Single 14-meter reflector used for testing of the main HERA telescope. (Under Construction) |
| Large Millimeter Telescope (LMT) | Sierra Negra,Puebla, Mexico | A 50-meter telescope for observations at millimetre wavelengths, the largest single dish instrument operating in this wavelength band. | |
| Leuschner Observatory | Lafayette, California, US | A 4.5-meter single dish, prototype dish for theAllen Telescope Array | |
| Long Wavelength Array (LWA) | Socorro, New Mexico, US | 10–88 MHz | A telescope composed of stations each with 256 crossed-dipole antennas operated by theUniversity of New Mexico and theNaval Research Laboratory. The first station (LWA1) is 50 miles west of Socorro, colocated with the VLA. The second station is at the Sevilleta National Wildlife Refuge 20 miles north of Socorro. Additional stations are planned. |
| Morehead State University 21m. | Morehead, Kentucky, US | A 21 m. telescope used for academic research and satellite data retrieval and control. | |
| Paul Plishner Radio Astronomy and Space Sciences Center | Haswell, Kiowa County, Colorado, US | An 18-meter telescope under development since 2010 for use by educators in Colorado and others. Sponsored by the Deep Space Exploration Society of Boulder County, Colorado | |
| Occidental College SRT (Small Radio Telescope), Hameetman Science Center | Los Angeles, California, US | A 2.3-meter satellite dish on a fully steerable, motorized azimuth-elevation mount with a low-noise amplifier and super-heterodyne receiver running SRT/VSRT (version 7.5). Currently inactive. | |
| OVRO 40 meter Telescope | Owens Valley Radio Observatory,Big Pine, California, US | 15 GHz | This cm wavelength telescope operated byCaltech, is currently being used on ablazar monitoring program at 15 GHz. |
| Owens Valley Solar Array | Owens Valley Radio Observatory,Big Pine, California, US | 1–18 GHz | This cm wavelength interferometric telescope operated byNew Jersey Institute of Technology, observes the solar corona from 1–18 GHz. |
| Peach Mountain Observatory | Ann Arbor, Michigan, US | 26m telescope built in 1958, operated by theUniversity of Michigan. Currently undergoing renovation. | |
| Precision Array for Probing the Epoch of Reionization (PAPER) | Green Bank, West Virginia, US | 100–200 MHz | Thirty-two crossed-dipole antennas measuring 100–200 MHz |
| Solar monitor, two 1.8 m dishes | Dominion Radio Astrophysical Observatory,Kaleden, British Columbia, Canada | The first dish here was originally a backup for the Algonquin site, but later the ARO instrument was moved to DRAO and this antenna became its backup. | |
| Stanford Dish, or theSRI International Antenna Facility | Palo Alto, California, US | 45.7 m parabolic reflector. Owned by theU.S. Government and constructed by SRI on land leased fromStanford University, the Antenna Facility is known locally as "The Dish". | |
| Synthesis Telescope, seven-elementinterferometer | Dominion Radio Astrophysical Observatory,Kaleden, British Columbia, Canada | ||
| Very Large Array (VLA) | Socorro, New Mexico, US | Array of 27dishes. Part of NRAO. | |
| Very Small Array (VSA) | Cogan Station, Pennsylvania, US | Array of 8 smalldishes. Part ofThe SETI League's Project Argus initiative. | |
| Very Long Baseline Array (VLBA) | Socorro, New Mexico US (operations center) | Array system of 10 radio telescopes; dishes are located atMauna Kea, Hawaii,Owens Valley, California,Brewster, Washington,Kitt Peak, Arizona,Pie Town, New Mexico,Los Alamos, New Mexico,Fort Davis, Texas,North Liberty, Iowa,Hancock, New Hampshire, andSt. Croix, U.S. Virgin Islands. | |
| Pisgah Astronomical Research Institute (PARI) | Rosman, North Carolina, US | 327 MHz, 1.4 and 4.8 GHz | Two 26m telescopes: 26 West and East. One 12m telescope, fully automated and accessed via PARI"s website. |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Atacama B-Mode Search (ABS) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 127–163 GHz | 60 cm telescope located on Cerro Toco and designed to measure the polarization of theCMB. |
| Atacama Cosmology Telescope (ACT) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 6 m telescope located on Cerro Toco. | |
| Atacama Large Millimeter Array (ALMA) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 35–950 GHz[51] | 54 dishes with 12-m diameter and 12 dishes with 7 m diameter, sensitive to wavelengths betweenradio andinfrared (submillimetre astronomy). |
| Atacama Pathfinder Experiment (APEX) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 159–738 GHz[52] | 12 m telescope located at the Chajnantor plateau. |
| Atacama Submillimeter Telescope Experiment (ASTE) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 270 GHz | 10 m telescope located at Pampa La Bola. This was a pathfinder instrument forALMA, and features an AzTEC millimeter camera in the focal plane of the dish, consisting of 144silicon nitride micromeshbolometer pixels arranged in a compact hexagonal package.[53] |
| Brazilian Decimetric Array (BDA) | Cachoeira Paulista,São Paulo, Brazil | 1.2–6.0 GHz | 38-element radio telescope interferometer working in the frequency range of 1.2–6.0 GHz. The final baseline will be 2.27 km in the east–west and 1.17 km in the South directions, respectively. This instrument will obtain radio images from the sun with a spatial resolution ≈4x6 arc seconds. Located in Cachoeira Paulista, São Paulo, Brazil (Latitude 45° 00' 20" West and Longitude 22° 41' 19" South)[54] |
| Cosmic Background Imager (CBI) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 13 dishes with 1 m diameter located at the Chajnantor plateau. Decommissioned in 2008. | |
| Itapetinga Radio Observatory | Atibaia, São Paulo, Brazil | 13.7 m telescope, operates in the K and Q bands, with cryogenic receivers[55] | |
| Jicamarca Radio Observatory (ROJ) | Lurigancho-Chosica,Lima Province, Peru | 50 MHz[56] | Main antenna is a cross-polarized square array composed of 18,432 half-wavelength dipoles. Research areas: Stable equatorial ionosphere, ionospheric field aligned irregularities, the dynamics of the equatorial neutral atmosphere and meteor physics.[57] |
| Cosmology Large Angular Scale Surveyor (CLASS) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 30–240 GHz[58] | Array of telescopes located on Cerro Toco and designed to measure the polarization of theCMB. |
| NANTEN2 Observatory (NANTEN2) | Llano de Chajnantor Observatory,Atacama Desert, Chile | 4 m telescope located at Pampa La Bola. | |
| Northeastern Space Radio Observatory | Eusébio, Brazil | 14.2 m telescope | |
| Polarization Emission of Millimeter Activity at the Sun | Complejo Astronomico El Leoncito (CASLEO),San Juan Province, Argentina | 45 and 90 GHz | Full sun disk patrols with left- and right-hand circular polarization receivers. |
| Q/U Imaging Experiment (QUIET) | Llano de Chajnantor Observatory,Atacama Desert, Chile | Located at the Chajnantor plateau. | |
| Solar Submillimeter Telescope (SST) | Complejo Astronomico El Leoncito (CASLEO),San Juan Province, Argentina | 212 GHz and 405 GHz | 1.5 m radome enclosed, single dishCassegrain antenna, with a focal array (4 beams @ 212 GHz, 2 beams @ 405 GHz) of room temperature receivers. |
| Swedish-ESO Submillimetre Telescope (SEST) | La Silla Observatory,Atacama Desert, Chile | 15 m telescope. Decommissioned in 2003[59] | |
| Estación de Espacio Lejano [es] | Neuquén Province, Argentina | S/X/Ka, Delta Dor | 35 m and 13.5 m Telescopes, Operated by Chinese Deep Space Network (CDSN) |
| Malargüe Station | Malargüe, Argentina | 35 m telescope and deep space antenna, operated byESTRACK |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Greenland Telescope | Thule Air Base,Greenland | 12 metre diameterCassegrain telescope. | |
| Eiscat Radio Telescope | Adventdalen, Svalbard | Studies of aurorae |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Very Small Array (VSA) | Observatorio del Teide,Canary Islands, Spain | Array of 14dishes, with two larger source-subtractiondishes. Controlled remotely from UK. | |
| Arecibo Telescope | Arecibo, Puerto Rico, US | 8–3,000 MHz | 305 m (1,001 ft) Second largest single dish spherical reflectorradiotelescope in the world. Structural issues led to the decision to dismantle the structure. Before this could be done the instrument platform collapsed in December 2020.[60] |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Mauritius Radio Telescope | Mauritius |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Caltech Submillimeter Observatory | Mauna Kea Observatory, Hawaii, US | 10.4 m (34 ft) diameter submillimeter wavelength telescope, closed since 2015, due to be dismantled since 2019 to return the land to the natives. | |
| James Clerk Maxwell Telescope | Mauna Kea Observatory,Hawaii, US | 86, 230, and 345 GHz | 15-meter submillimetre-wavelength telescope operated by theJoint Astronomy Centre |
| Submillimeter Array (SMA) | Mauna Kea Observatory, Hawaii, US | 180–420 GHz | Operated jointly by theSmithsonian Astrophysical Observatory and theAcademia Sinica Institute of Astronomy and Astrophysics of Taiwan. |
| Warkworth Radio Telescope | Warkworth Radio Observatory,Warkworth, New Zealand | 1.2–21 GHz | 12 metre fully steerable dish operated by IRASR,Auckland University of Technology[61] |
| Warkworth 2 dish | Warkworth Radio Observatory,Warkworth, New Zealand | 6–21 GHz | 30 metre fully steerable dish operated by IRASR, AUT University[61] |
| Transient Array Radio Telescope | Signal Hill,Dunedin, New Zealand | 1.575 GHz | 24-element aperture synthesis open source all-sky radio telescope,[62] designed and developed by theUniversity of Otago. |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| HALCA (Highly Advanced Laboratory for Communications and Astronomy) | Earth orbit with anapogee altitude of 21,400 km and aperigee altitude of 560 km. | Ceased operations 2005 | |
| Spektr-R or RadioAstron | 10 meter radio telescope in a highly elliptical earth orbit. Launched July 2011. | Ceased operations 2019 | |
| Queqiao | Chinese Earth-Moon L2 orbiter | ||
| Chang'e 4 | Chinese base on far side of Moon | ||
| Queqiao-2 | Chinese lunar orbiter |
| Name | Location | Frequency Range | Remarks |
|---|---|---|---|
| Deep Synoptic Array | Nevada,United States | 0.7–2.0 GHz | An array of 1650 6.15-meter dishes designed for sky surveys. Expected to start operation in 2029. |
| EAARO - East Anglian Astrophysical Research Organisation | Cambridgeshire, England[39] | 0–11 GHz | A scientific and educational charitable company currently constructing a Radio Observatory and Ground Station in Cambridgeshire |
| Large Latin American Millimeter Array (LLAMA) | Alto Chorrillos, near San Antonio de los Cobres,Salta, Argentina | 45–900 GHz | 12 m single dish, VLBI, in construction, expected to start operations in 2017 |
| Qitai 110m Radio Telescope (QTT) | Xinjiang, China | 0.3–117 GHz | Planned world's largest fully steerable single-dish radio telescope with a diameter of 110 meters. Operates at 300 MHz to 117 GHz. Construction of the telescope is planned to start in 2013 and completed within 10 years.[63][64] |
| Square Kilometer Array (SKA-Phase1) | Carnarvon, South Africa | L-Band,X-Band,S-Band,UHF | Additional 128 dishes merged with MeerKAT, expected to be operational in 2022. |
| Baryon Acoustic Oscillations in Integrated Neutral Gas Observations (BINGO) | Aguiar, Paraíba, Brazil | 980–1260 MHz | Acrossed-dragone telescope with a 20 m main semi-axis primary reflector and a 17.8 m main semi-axis secondary reflector with 28 receivers, dedicated mainly to the detection of theBaryon Acoustic Oscillations through the21 cm emission line.[65] |
| THERMOpYlae | Phthiotis, Greece | 32 metre (104 ft.) single dish communication antenna being converted into a radio telescope by theUniversity of Thessaly and theHellenic Open University.[66] |
| Name | Location | Frequency Range | Remarks | |
|---|---|---|---|---|
| 30m Sub-Millimeter Telescope (TSMT) | China | A 30m aperture sub-millimeter telescope (TSMT) with an active reflector has been proposed in China.[67] | ||
| LOFAR Super Station (LSS) | Nançay, France | 10–80 MHz | The Nancay radio astronomy observatory and associated laboratories are developing the concept of a "Super Station" for extending theLOFAR station now installed and operational in Nancay. The LOFAR Super Station (LSS) will increase the number of high sensitivity long baselines, provide short baselines and an alternate core, and be a large standalone instrument. It will operate in the low frequency band of LOFAR (30–80 MHz) and extend this range to lower frequencies. | |
| Lunar Crater Radio Telescope (LCRT) | Moon | Below 30 MHz | The Lunar Crater Radio Telescope (LCRT) is a proposal by the NASA Institute for Advanced Concepts to create an ultra-long-wavelength (hereby wavelengths greater than 10 m – i.e., frequencies below 30 MHz) radio telescope inside a lunar crater on the far side of the Moon. | |
| Square Kilometer Array (SKA-Phase2) | Australia, South Africa | 0.05–30 GHz | Extension of SKA-Phase to approximately 2000 dishes. This array, if built, would be 50 times more sensitive and 10,000 times faster than any other radio telescope. | |
| Hongmeng Project (DSL) | lunar orbit | 0.1–30 MHz imaging, 0.1–120 MHz global spectrum | The Hongmeng project, also known as the Discovering Sky at the Longest wavelength (DSL) project is a Chinese space mission concept to create an ultra-long-wavelength radio telescope array on an orbit around the Moon. |
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