List of radio telescopes#Space-based

|Kuntunse, Ghana

| 3.8–6.4, 5, 6.7 GHz

| 32-metre (104 foot) single dish, first of African VLBI Network{{cite web | url=http://www.ska.ac.za/media-releases/ghana-and-south-africa-celebrate-first-success-of-african-network-of-telescopes/ | title=C-BASS|website=Ska.ac.za }}

|Meerkat National Park, South Africa

| 4.5–5.5 GHz

| 7.6-metre (24.9 foot) dish with polarimeter back end{{cite web | url=http://www.astro.caltech.edu/cbass/ | title=C-BASS|website=Astro.caltech.edu }}

| Hartebeesthoek Radio Astronomy Observatory, Johannesburg, South Africa

| 1.66–23 GHz

| 26 m dish.{{cite web | url=http://www.hartrao.ac.za/factsfile.html | title=HartRAO Radio Telescope Facts |website=Hartrao.ac.za| access-date=2007-01-23}}

| Hartebeesthoek Radio Astronomy Observatory, Johannesburg, South Africa

| 2.3–8.65 GHz

| 15 m Experimental Demonstrator Model originally build as a technology demonstrator for MeerKAT{{cite news|url=http://www.engineeringnews.co.za/article/this-year-will-see-major-advances-in-sa-and-international-radio-astronomy-projects-2010-01-15|title=This year will see major advances in South Africa and in international radio astronomy projects |date=2010-01-15|publisher=Engineering News (Creamer Media)|access-date=5 April 2010}}

|Meerkat National Park, South Africa

| 50–200 MHz

| In progress – currently nineteen 14 m reflectors with crossed dipole antennas as feed.

|Meerkat National Park, South Africa

| 400–800 MHz

| In progress – currently eight 6 m dishes with dual-polarization dipole antennas as feed at HartRAO.

| Durban University of Technology, Durban, South Africa

| 1420 MHz

| 5 meter (16 foot) parabolic reflector{{cite web|url=http://indlebe.dut.ac.za/|title=Indlebe|publisher=Durban University of Technology|access-date=5 April 2010|archive-url=https://web.archive.org/web/20120305140655/http://indlebe.dut.ac.za/|archive-date=5 March 2012|url-status=dead}}

| Meerkat National Park, South Africa

| 1200–1950 MHz

| Seven, 12 meter (39 foot) dishes.

| Meerkat National Park, South Africa

| 0.58–14.5 GHz

| Sixty four, 13.5 m dishes. A pathfinder for the Square Kilometre Array.{{cite web|url=http://www.ska.ac.za/kat/index.shtml |title=About the KAT |access-date=2007-01-23 |archive-url=https://web.archive.org/web/20070208142951/http://www.ska.ac.za/kat/index.shtml |archive-date=2007-02-08 |url-status=dead }}

|Meerkat National Park, South Africa

| 100–200 MHz

| Now disassembled, PAPER at its maximum had 128 crossed dipole antennas,{{cite web|url=https://www.sarao.ac.za/newsletters/sarao-news/02-2018/paper-a-precursor-to-hera/ |title=PAPER a precursor to HERA }} making it the interferometer with more elements than any other at that time.

| Amundsen–Scott South Pole Station

| 26–36 GHz

| 13-element interferometer measuring anisotropies in the cosmic microwave background.{{cite web | url=http://astro.uchicago.edu/dasi/ | title=Degree Angular Scale Interferometer | website=Astro.uchicago.edu | access-date=4 January 2009 | archive-url=https://web.archive.org/web/20101210122303/http://astro.uchicago.edu/dasi/ | archive-date=10 December 2010 | url-status=dead }}

| Amundsen–Scott South Pole Station

| 95–350 GHz

| 10-m microwave telescope making observations of clusters using the Sunyaev-Zeldovich effect.{{cite web | url=http://pole.uchicago.edu/index.php |title=South Pole Telescope|website=Pole.uchicago.edu |access-date=4 January 2009}} Also participates in Event Horizon Telescope observations.

| Delingha, Qinghai, China

| 85–115 GHz

| Dish diameter: 13.7 m. Site altitude: 3200 m. Operated by Purple Mountain Observatory.

| Shanghai, China

| 1660 MHz

| 25 m. Operated by SHAO (Shanghai Astronomical Observatory)

| Ürümqi, China

| 1.4–18 GHz

| L/C/S/X band receivers. 70 km south to Ürümqi. Operated by XAO (Xinjiang Astronomical Observatory).

| 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.

| 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.{{cite web|url=https://www.eurekalert.org/zh/?story=20081104.CSRH|title=最新消息 – EurekAlert! 優睿科 – EurekAlert! Science News|website=Eurekalert.org|access-date=14 December 2018}}{{cite web|url=http://www.atnf.csiro.au/research/Astro2008/Postings/Na_Wang.pdf|title=Large Radio Telescopes In China : Na Wang|website=Atnf.csiro.au|access-date=14 December 2018}}

| Miyun, China

| 232 MHz

| Array of 28 9-meter dishes, completed in 1984.

| Miyun, China

| 2–12 GHz

| Built in 2005.

| Kunming, China

| 2–12 GHz

| Built in 2006.

| 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

| Hongliuxia, Balikun, Xinjiang, China

| 500-1500 adjustable, currently 700-800 MHz

| 16 dishes of 6m aperture, built in 2016

| Shanghai, China

| 1–50 GHz

| Built in 2012.{{cite web|url=http://news.xinhuanet.com/english/photo/2012-03/12/c_131462629.htm|archive-url=https://web.archive.org/web/20150604095412/http://news.xinhuanet.com/english/photo/2012-03/12/c_131462629.htm|url-status=dead|archive-date=4 June 2015|title=Radio telescope under construction in Shanghai |website= Xinhua – English.news.cn|date=4 June 2015|access-date=14 December 2018}} Operated by SHAO (Shanghai Astronomical Observatory)

| Pune, Maharashtra, India

| 50–1420 MHz

| Thirty 45 m wire dishes;{{cite web | url=http://www.gmrt.ncra.tifr.res.in/gmrt_hpage/GMRT/intro_gmrt.html | title=Introducing GMRT|website=Gmrt.ncra.tifr.res.in | access-date=2007-01-23}} largest telescope at meter wavelengths. Operated by the National Centre for Radio Astrophysics.{{cite web | title=Giant Metrewave Radio Telescope, Tata Institute of Fundamental Research | url=http://www.gmrt.ncra.tifr.res.in/|website=Gmrt.ncra.tife.res.in}}

| Ooty, Tamil Nadu, India

| 326.5 MHz

| The radio telescope is a 530-metre (1,740 ft) long and 30-metre (98 ft) tall cylindrical parabolic antenna. It operates at a frequency of 326.5 MHz with a maximum bandwidth of 15 MHz at the front end.

| Gauribidanur, Karnataka, India

| 40–150 MHz

| Operated by (Indian Institute of Astrophysics). A Radioheliograph.

| 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 the National Astronomical Observatory of Japan (NAOJ)

| 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).{{cite web|url=http://wikimapia.org/2093308/Siberian-Solar-Radio-Telescope-SSRT|title=Siberian Solar Radio Telescope (SSRT)|website=Wikimapia.org|access-date=14 December 2018}}

| Badary, Buryatia, Russia

| 1.4–22 GHz

| 32 m RT-32 radio telescope, operating range 1.4–22 GHz.{{Cite web |url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/20080032653_2008032998.pdf |title=Archived copy |access-date=2017-07-07 |archive-url=https://web.archive.org/web/20100214225429/http://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/20080032653_2008032998.pdf |archive-date=2010-02-14 |url-status=dead }}

| Galenki (Ussuriysk), Russia

| 5–300 GHz

| RT-70, 70 m telescope, operating range 5–300 GHz

| Suffa plateau, Uzbekistan

| 5–300 GHz

| RT-70, the construction started in 1981 but was never completed.

|Guizhou, China

|70–3000 MHz

|500m radio telescope, the world's largest filled-aperture radio telescope, operating range 70–3000 MHz.{{cite web|url=http://fast.bao.ac.cn/en/FAST.html|archive-url=https://web.archive.org/web/20170316160050/http://fast.bao.ac.cn/en/FAST.html|url-status=dead|archive-date=16 March 2017|date=16 March 2017|access-date=14 December 2018|title=FAST - Homepage }}

| Qitai County, Xinjiang, China

| 300 MHz–117 GHz

| Construction work started in 2012. Will be operated by XAO (Xinjiang Astronomical Observatory).

| Chiang Mai, Thailand

| 300 MHz–115 GHz

| Construction work started in 2017. A 40m single-dish short-millimetre telescope,https://radio.kasi.re.kr/eavn/images/presentation/10.Kitiyane_Asanok.pdf {{Bare URL PDF|date=March 2022}} operated by the National Astronomical Research Institute of Thailand (NARIT).{{Cite web |url=http://www.narit.or.th/en/index.php/news/575-thai-german-relation-wafts-as-40-meter-radio-telescope |title=National Astronomical Research Institute of Thailand (Public Organization) - Thai – German relation wafts as 40-meter Radio Telescope pinpointed in Chiang Mai |access-date=2019-06-23 |archive-date=2019-06-23 |archive-url=https://web.archive.org/web/20190623030130/http://www.narit.or.th/en/index.php/news/575-thai-german-relation-wafts-as-40-meter-radio-telescope |url-status=dead }}

| Japan

| 6.7 GHz–43 GHz

| A VLBI system with four 20-m telescopes in Japan (Mizusawa, Chichijima, Iriki, Ishigaki island){{Cite web|title=Toppage - VERA|url=https://www.miz.nao.ac.jp/veraserver/index.html|access-date=2021-09-21|website=www.miz.nao.ac.jp}} operated by the National Astronomical Observatory of Japan (NAOJ).

| Sichuan province, China

| 150 MHz–450 MHz

| 313 parabolic antennas for detection of coronal mass ejection events. Operations started in 2023.{{cite web |title=China's new radio telescope will have dangerous solar eruptions in its gaze |url=https://www.scmp.com/news/china/science/article/3184087/chinas-new-radio-telescope-will-have-dangerous-solar-eruptions |website=South China Morning Post |access-date=26 July 2023 |language=en |date=5 July 2022}}

| Inner Mongolia, China

| 327 MHz and 654 MHz{{cite journal |last1=Yan |first1=Yihua |last2=Wang |first2=Wei |last3=Chen |first3=Linjie |last4=Liu |first4=Fei |last5=Fan |first5=Jin |last6=Chen |first6=Zhijun |last7=Geng |first7=Lihong |last8=Tan |first8=Chengming |last9=Ma |first9=Suli |last10=Li |first10=Sha |last11=Su |first11=Cang |last12=Du |first12=Jing |last13=Cheng |first13=Jun |last14=Zhu |first14=Xiaoshuai |last15=Zhou |first15=Zhichao |last16=Zhang |first16=Minghui |display-authors=1 |title=MUSER and IPS telescopes for solar and space weather observations |journal=Advances in Space Research |date=8 March 2023 |doi=10.1016/j.asr.2023.03.003 |s2cid=257473011 |url=https://www.sciencedirect.com/science/article/abs/pii/S0273117723001953 |language=en |issn=0273-1177|url-access=subscription }}

| interplanetary scintillation telescope, consists of three rotatable cylindrical antennas (140 metres by 40 metres each).{{cite web |title=China to start building giant telescope to monitor solar winds |url=https://www.scmp.com/news/china/science/article/3183412/china-start-building-giant-telescope-monitor-solar-winds-can |website=South China Morning Post |access-date=27 July 2023 |language=en |date=29 June 2022}}

| 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{{Cite web|url=https://www.kasi.re.kr/main.php|title= Korea Astronomy and Space science Institute (KASI)}} (KASI). It is operated by Radio astronomy division in KASI.{{Cite web|url=https://radio.kasi.re.kr/main.php|title=Radio astronomy division in KASI|date=13 September 2023}}

| Republic of Korea

| 22/43/86/129 GHz

|KVN consists of four 21-m radio telescopes located in Seoul, Ulsan, Jeju Island and Pyeongchang (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.{{Cite web|url=https://kvn.kasi.re.kr/main.php|title=Korean VLBI Network (KVN)|date=13 September 2023}}

| Murchison Radio-astronomy Observatory, Western Australia

| 700–1800 MHz

| [http://www.atnf.csiro.au/projects/askap/ ASKAP], the Australian Square Kilometre Array Pathfinder, is operated by CSIRO. It is made up of 36 identical antennas, each 12 metres in diameter, with a 30 sq degrees FoV at 1.4 GHz.{{cite web | title=Australian Square Kilometre Array Pathfinder| url=https://www.atnf.csiro.au/projects/askap/}}

| Paul Wild Observatory, Narrabri, New South Wales

| 0.3–110 GHz

| 6x22m dish aperture synthesis array, operated by CSIRO as part of the ATNF (Australia Telescope National Facility).{{cite web | title=Australia Telescope Compact Array | url=http://www.narrabri.atnf.csiro.au/|website=Narrabri.atnf.csiro.au}}

| Tidbinbilla, Australian Capital Territory

|

| 1x70 m dish, 3x34 m dishes, operated by CSIRO on behalf of NASA.{{cite web | title=Canberra Deep Space Communication Complex | url=http://www.cdscc.nasa.gov/Pages/trackingtoday.html|website=Cdscc.nasa.gov}}

| Ceduna, South Australia

| 1.2–23 GHz

| 30 m telescope, operated by the University of Tasmania

| Molonglo (near Canberra, Australian Capital Territory)

| 600–1200 MHz

| Operated by the School of Physics at the University of Sydney. East-west arm of the former Molonglo Cross Telescope, approximately 1.6 km in length. Operates at 843 MHz.

| Mopra Observatory, near Coonabarabran, New South Wales

| 0.3–100 GHz

| 22 m dish, operated by CSIRO as part of the ATNF (Australia Telescope National Facility).{{cite web | title=Mopra telescope | url=http://www.narrabri.atnf.csiro.au/mopra/|website=Narrabri.atnf.csiro.au| date=6 April 2021}}

| Hobart, Tasmania

| 1.2–23 GHz

| 26 m telescope, operated by the University of Tasmania

| 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 Observatory, New South Wales

|

| 64 m telescope (2nd largest movable dish in the Southern Hemisphere), operated by CSIRO as part of the ATNF (Australia Telescope National Facility).{{cite web|url=http://www.parkes.atnf.csiro.au/|title=CSIRO Parkes Observatory – Australia Telescope National Facility|website=Parkes.atnf.csiro.au|access-date=14 December 2018}}

| Bad Münstereifel-Effelsberg near Bonn, Germany

| 395 MHz – 95 GHz

| 100 m fully steerable dish operated by Max Planck Institut für Radioastronomie, operates at 395 MHz to 95 GHz

| Volokhiv Yar, Kharkiv, Ukraine

| 8–33 MHz

| World's largest radio telescope at decametre wavelengths (max. collective area 150,000 m²).

| 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.

| Jodrell Bank Observatory, Cheshire, England

|0–2 GHz

| 76 m dish

| former soviet Center for deep space communications, Yevpatoria, Crimea

| 5–300 GHz

| RT-70, 70 m telescope, operating range 5–300 GHz

| Zelenchukskaya, Russia

| 0.61–30 GHz

| 600 m dish, operates at 610 MHz to 30 GHz, world's largest diameter individual radio telescope

| Kalyazin, Russia{{cite web |url=http://www.okbmei.ru/en/page.html?id=54 |title=Archived copy |access-date=2008-08-14 |url-status=dead |archive-url=https://web.archive.org/web/20081226041319/http://www.okbmei.ru/en/page.html?id=54 |archive-date=2008-12-26 }}

| 5.86 GHz

| 64 m fully steerable dish, up to 5.86 GHz

| Medvezhji Ozera (Bear Lakes), Russia

| 5.86 GHz

| 64 m fully steerable dish, up to 5.86 GHz

| 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 the Pushchino Radio Astronomy Observatory.

| 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 the Pushchino Radio Astronomy Observatory.{{cite web|url=http://iopscience.iop.org/1063-7869/52/11/R09/pdf/1063-7869_52_11_R09.pdf|title=The Pushchino Radio Astronomy Observatory of the P N Lebedev Physical Institute Astro Space Center: yesterday, today, and tomorrow|website=Iopscience.iop.org|access-date=14 December 2018}}

| 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 the Pushchino Radio Astronomy Observatory.

| Karachaevo-Cherkessiya, Russia

| 1.4–22 GHz

| 32m RT-32 radio telescope, operating range 1.4–22 GHz. [ftp://ivscc.gsfc.nasa.gov/pub/annual-report/2009/pdf/nszel.pdf]{{dead link|date=May 2025|bot=medic}}{{cbignore|bot=medic}}

| Svetloe, Karelia, Russia

| 1.4–22 GHz

| 32m RT-32 radio telescope, operating range 1.4–22 GHz.{{Cite web |url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/20080032644_2008032993.pdf |title=Archived copy |access-date=2017-07-07 |archive-url=https://web.archive.org/web/20100513054408/http://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/20080032644_2008032993.pdf |archive-date=2010-05-13 |url-status=dead }}

| Moscow Oblast, Russia

|

| Two 7.75-meter diameter antennas (only one is working at the moment){{cite web|url=http://lud.bmstu.ru/english_RT/index.htm|title=Welcome to the site of one of the unique millimeter-range Radiotelescope!|website=Lud.bmstu.ru|access-date=14 December 2018}}

| Spanish National Observatory, Yebes, Guadalajara, Spain{{cite web|url=http://www.oan.es/|title=Infraestructuras y trabajos de Astronomía del Instituto Geográfico Nacional|website=Oan.es|access-date=14 December 2018}}

|

| 40 m parabolic steerable telescope for mm and cm wavelengths

| Toruń Centre for Astronomy, Toruń, Poland

|

| RT4 (32 m) parabolic antenna

| Ventspils International Radio Astronomy Center, Irbene, Latvia

|

| 32-meter fully steerable parabolic, centimetre-wave range antenna RT-32{{cite web|url=http://www.meteoriti.lv/|title=Meteoriti.LV|website=Meteoriti.lv|access-date=14 December 2018}}

| Medicina Radio Observatory, Medicina, Bologna, Italy{{cite web|url=http://www.ira.inaf.it/Home.html|title=IRA Home|website=Ira.inaf.it|access-date=14 December 2018}}

| 408 MHz

| 32000 m² interferometer, cylindrical-paraboloid steerable over NS., 408 MHz, Beam=3'

| Medicina Radio Observatory, Medicina, Bologna, Italy

| 1.4–43 GHz

| 32 m, fully steerable dish, 1400 MHz...43 GHz

| Noto Radio Observatory, Noto, Italy,

| 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.

| United Kingdom

|151 MHz – 24 GHz

| Consists of the Cambridge 32 m at Mullard Radio Astronomy Observatory, Darnhall, Defford, Tabley (also known as Pickmere) and Knockin. Also includes the Lovell and Mark II telescopes at Jodrell Bank.

|Cambridgeshire, England{{cite web|url=http://www.eaaro.org.uk/|title=EAARO|website=Eaaro.org.uk|access-date=14 December 2018}}

| 0–11 GHz

| A scientific and educational charitable company currently constructing a Radio Observatory and Ground Station in Cambridgeshire

| Center for deep space communications, Simferopol, Crimea

|

| {{Interlanguage link multi|TNA-400|ru|3=ТНА-400}}, 32 m telescope

| Pico Veleta, in Granada, 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 with superheterodyne and bolometric detectors.

| Jodrell Bank Observatory, Cheshire, England

|0–24 GHz

| 25 m dish

| Bad Münstereifel-Eschweiler near Bonn, Germany

|

| 25 m dish operated by University of Bonn and Max Planck Institut für Radioastronomie, closed in 1993, now owned by NRW-Stiftung,{{cite web|url=https://www.nrw-stiftung.de/index.php|title=NRW-Stiftung – Aktuelle News und Projekt der Woche: Schloss Harkotten im Munsterland|website=Nrw-stiftung.de|access-date=14 December 2018}} reopened 2010 after restoration and operated by Förderverein Astropeiler Stockert{{cite web|url=https://www.astropeiler.de/|title=Astropeiler Stockert e.V. – Radioastronomie, Amateurfunk, Natur und mehr|website=Astropeiler.de|access-date=14 December 2018}}

| Toruń Centre for Astronomy, Toruń, Poland

|

| RT3 (15 m) antenna.

| Westerbork, Netherlands

|

| 2.8 km array of 14 25-meter dishes operated by ASTRON

| Onsala Space Observatory, Onsala, Sweden

|

| 25 m telescope

| Dwingeloo, Netherlands

|

| 25 m steerable dish, formerly operated by ASTRON, now operated by CAMRAS{{cite web|url=https://www.camras.nl/|title=Dwingeloo Radiotelescoop – CAMRAS – C.A. Muller Radioastronomie Station – PI9CAM|website=Camras.nl|access-date=14 December 2018}}

| 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.

| Onsala Space Observatory, Onsala, Sweden

|

| 20 m telescope

| Center for deep space communications, Yevpatoria, Crimea

|

| 8 mirrors with diameter of 16 meters. Square is 1000 sq. meters.

| Ventspils International Radio Astronomy Center, Irbene, Latvia

|

| 16-meter diameter antenna RT-16

| Kilpisjärvi, Enontekiö, Finland

|

| 30 m × 50 m, 768-element phased array and a 34 m diameter, 48-element phased array

| Kylmälä, Kirkkonummi, Finland

| 2–150 GHz

| 13.7 m dish, operates at 2 to 150 GHz, surface accuracy 0.1 mm (rms).

| Mullard Radio Astronomy Observatory, Cambridge, England

|

| Eight 13 m dishes, and is currently used as one part of the Arcminute Microkelvin Imager.

| Kayseri, Turkey

|

| 12.8 m dish

| 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{{Cite web |url=http://serveurwurzburg.obs.u-bordeaux1.fr/ |title=Wurzburg v2.0 |access-date=2013-05-10 |archive-url=https://web.archive.org/web/20130510232103/http://serveurwurzburg.obs.u-bordeaux1.fr/ |archive-date=2013-05-10 |url-status=dead }}

| Distributed across Europe with members in China, South Africa and the US

|

| VLBI array operated by the European Consortium for VLBI

| Plateau de Bure, Grenoble, France

|

| Originally an array of 3 antennas, since 2005 has 6 antennas, operating at millimeter wavelengths, now part of NOEMA

| Plateau de Bure, Grenoble, France

|

| 12 antennas, operating at millimeter wavelengths (Operational: 2019).

| Nançay, France

|

| [https://web.archive.org/web/20130103184107/http://www.obs-nancay.fr/en/index.php/instruments/radio-telescope NRT website (fr)]

| Nançay, France

| 10–100 MHz

| [https://web.archive.org/web/20130124085028/http://www.obs-nancay.fr/en/index.php/instruments/decametric-array DAM website (fr)]

| Nançay, France

| 150–450 MHz

| [https://web.archive.org/web/20130105202839/http://www.obs-nancay.fr/en/index.php/instruments/radio-heliograph NRH website (fr)]

| Germany

|

| A Small Network of Radio Telescopes and Radio Spectrographs doing Amateur Radio Astronomy at a Very High standard coordinated by The European Radio Astronomy Club{{cite web|url=http://www.eracnet.org/|title=ERAC – The European Radio Astronomy Club|website=Eracnet.org|access-date=14 December 2018}} Research and Development Telescope in Mannheim Germany.

| 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 by ASTRON

| São Gião, Portugal

| 0.4–22 GHz

| 9.3 m solid surface dish, operated by PARAC{{cite web | url=http://parac.eu | title=PARAC |website=parac.eu|access-date=18 January 2019}}

| Mullard Radio Astronomy Observatory, Cambridge, England

|

| Small Array consists of 10 3.7-m parabolic antennas

| Mannheim, Germany

|

| From 14 kHz VLF up to 40 GHz{{cite web|url=http://www.eracnet.org/home|title=Radio Telescope Mannheim|website=Eracnet.org|access-date=14 December 2018}}{{Dead link|date=March 2020 |bot=InternetArchiveBot |fix-attempted=yes }}

| The European Radio Astronomy Club, Elsass, France

|

| Phased array and Digital back end based on the SKA design

| The European Radio Astronomy Club, East Lothian, Scotland

|

| Phased array and Digital back end based on the SKA design

| San Basilio, Sardinia, Italy

|

|Sardinia Radio Telescope. 64 m dish.

| Mount Aragats, Armenia, near Yerevan

| 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.Archived at [https://ghostarchive.org/varchive/youtube/20211205/SI57x_o5vnc Ghostarchive]{{cbignore}} and the [https://web.archive.org/web/20190524235119/https://www.youtube.com/watch?v=SI57x_o5vnc Wayback Machine]{{cbignore}}: {{cite web| url = https://www.youtube.com/watch?v=SI57x_o5vnc| title = URBEX {{!}} Epic abandoned Soviet radio telescope | website=YouTube}}{{cbignore}}

| Hertfordshire, UK

| 1.4 GHz

| 4.5 m single dish, and 115 m baseline 3 dish interferometer. Operated by the University of Hertfordshire

| Algonquin Radio Observatory, Algonquin Park, Ontario, Canada

|

| 46 metre fully steerable dish operated by Thoth Technology,{{cite web|url=http://169.48.13.120/|title=Home – Thoth Technology|website=169.48.13.120|access-date=14 December 2018|archive-date=14 December 2018|archive-url=https://web.archive.org/web/20181214213845/http://169.48.13.120/|url-status=dead}} Canada's largest radio telescope.

| Hat Creek Radio Observatory, Hat Creek, California, US

| 0.5–11.5 GHz

| 42 6-m gregorian offset dishes using log periodic cooled feed covering 0.5–11.5 GHz. Operated by joint agreement between SRI International and the SETI Institute

| Kitt Peak National Observatory, Tucson, Arizona, US

|

| Previously operated by the NRAO, this telescope is currently operated by the University of Arizona's Arizona Radio Observatory, part of Steward Observatory.

|Owens Valley Radio Observatory, Big Pine, California, US

| 4.5–5.5 GHz

| 6.1 metre dish with polarimeter back end. This telescope was decommissioned in April 2015.

| Dominion Radio Astrophysical Observatory, Kaleden, British Columbia, Canada

|400–800 MHz

| A novel drift scan telescope, which consists of four 100 × 20 meter 5 m focal length cylinders, with an array of 256 dual-polarized radio receivers along the focus. Will map the 21 cm line of neutral hydrogen over the cosmological redshift range of 0.8 to 2.5. Collected its first light in September 2017.{{Cite web |url=https://casca.ca/?p=9453| title=CHIME First Light| date=September 18, 2017|access-date=2020-11-25}}

| Center for Astrophysics {{!}} Harvard & Smithsonian, Cambridge, Massachusetts, USA

|115 GHz

|A small radio telescope which, along with a twin instrument in Chile, has been continuously mapping interstellar carbon monoxide since the 1970s.

|Owens Valley Radio Observatory, Big Pine, California, US

| 75–345 GHz

|Heterogeneous interferometer array composed of 6 10-m elements, 9 6-m elements, and 8 3.5-m elements covering frequencies ranging from 27–36 GHz, 80–115 GHz, and 215–265 GHz. Operated by joint agreements between Radio Astronomy Laboratory University of California, Berkeley, Caltech, University of Maryland, College Park, University of Illinois Urbana-Champaign, and the University of Chicago.

|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

| Kaleden, British Columbia, Canada

|408–1420 MHz

| Synthesis telescope consists of seven {{convert|9|m|ft|adj=on}} parabolic antennas, three of which are movable along a 600-metre rail line.

| Owens Valley Radio Observatory, Big Pine, California, US

| 1280-1530 MHz

| Array of 110 dishes of 5 meter diameter. Optimized for detecting and localizing fast radio bursts.

| Amherst, Massachusetts, US

|

| Operated by UMass Amherst

|Mojave Desert, California, US

|

|One of the most sensitive radars in the world

| Green Bank, West Virginia, US

|

| Three {{convert|26|m|ft|abbr=off|sp=us}} radio telescopes formerly operated by NRAO, and now kept by GBO as a historic telescope.

| 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 {{convert|100|m|ft|adj=on}} fully steerable single-dish radio telescope

| 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.{{cite web|url=https://greenbankobservatory.org/science/telescopes/140-foot/|title=Green Bank Observatory, 140 foot Telescope |access-date=2020-09-02}}

|Green Bank, West Virginia, US

|

|20m telescope, fully automated and accessed through the University of North Carolina's [https://skynet.unc.edu/ Skynet Robotic Telescope Network].

| 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 the Massachusetts Institute of Technology

| Mount Graham, Arizona, US

|

| 10-meter radio telescope operated by the University of Arizona's Arizona Radio Observatory, part of Steward Observatory.

|Embry-Riddle Radio Observatory, Prescott AZ, US

|100–200 MHz

|Single 14-meter reflector used for testing of the main HERA telescope. (Under Construction)

| Sierra Negra, Puebla, Mexico

|

| A 50-meter telescope for observations at millimetre wavelengths, the largest single dish instrument operating in this wavelength band.

| Lafayette, California, US

|

| A 4.5-meter single dish, prototype dish for the Allen Telescope Array

|Socorro, New Mexico, US

|10–88 MHz

| A telescope composed of stations each with 256 crossed-dipole antennas operated by the University of New Mexico and the Naval 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, Kentucky, US

|

| A 21 m. telescope used for academic research and satellite data retrieval and control.

|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

|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.

|Owens Valley Radio Observatory, Big Pine, California, US

| 15 GHz

|This cm wavelength telescope operated by Caltech, is currently being used on a blazar monitoring program at 15 GHz.

|Owens Valley Radio Observatory, Big Pine, California, US

| 1-18 GHz

|This cm wavelength interferometric telescope operated by New Jersey Institute of Technology, observes the solar corona from 1-18 GHz.

|Ann Arbor, Michigan, US

|

| 26m telescope built in 1958, operated by the University of Michigan. Currently undergoing renovation.

|Green Bank, West Virginia, US

| 100–200 MHz

| Thirty-two crossed-dipole antennas measuring 100–200 MHz

| 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.

| Palo Alto, California, US

|

| 45.7 m parabolic reflector. Owned by the U.S. Government and constructed by SRI on land leased from Stanford University, the Antenna Facility is known locally as "The Dish".

| Dominion Radio Astrophysical Observatory, Kaleden, British Columbia, Canada

|

| 

| Socorro, New Mexico, US

|

| Array of 27 dishes. Part of NRAO.

| Cogan Station, Pennsylvania, US

|

| Array of 8 small dishes. Part of The SETI League's Project Argus initiative.

| Socorro, New Mexico US
(operations center)

|

| Array system of 10 radio telescopes; dishes are located at Mauna 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, and St. Croix, U.S. Virgin Islands.

| 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.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

| 127–163 GHz

| 60 cm telescope located on Cerro Toco and designed to measure the polarization of the CMB.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

|

| 6 m telescope located on Cerro Toco.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

| 35-950 GHz{{cite web | url=https://almascience.eso.org/about-alma/alma-basics | title=ALMA Basics }}

| 54 dishes with 12-m diameter and 12 dishes with 7 m diameter, sensitive to wavelengths between radio and infrared (submillimetre astronomy).

| Llano de Chajnantor Observatory, Atacama Desert, Chile

| 159–738 GHz{{cite web|title=APEX instrumentation |url=http://www.apex-telescope.org/instruments/

|publisher=APEX |date=2018 |access-date=2020-06-21

}}

| 12 m telescope located at the Chajnantor plateau.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

| 270 GHz

| 10 m telescope located at Pampa La Bola. This was a pathfinder instrument for ALMA, and features an AzTEC millimeter camera in the focal plane of the dish, consisting of 144 silicon nitride micromesh bolometer pixels arranged in a compact hexagonal package.{{Cite web|url=http://www.lmtgtm.org/telescope/instrumentation/instruments/aztec/?lang=en|title=LMT – Large Millimeter Telescope Alfonso Serrano|website=www.lmtgtm.org|language=en|access-date=2019-11-10}}

| 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){{cite web | url=http://www.das.inpe.br/fmi/bda/| title=Brazilian Decimetric Array (BDA)|website=Das.inpe.br | access-date=2010-01-28}}

| Llano de Chajnantor Observatory, Atacama Desert, Chile

|

| 13 dishes with 1 m diameter located at the Chajnantor plateau. Decommissioned in 2008.

| Atibaia, São Paulo, Brazil

|

| 13.7 m telescope, operates in the K and Q bands, with cryogenic receivers{{cite web|url=http://www.das.inpe.br/radio/observatorio.html |title=Radio Observatorio do Itapetinga (ROI) |access-date=2010-01-28 |url-status=dead |archive-url=https://web.archive.org/web/20100723125544/http://www.das.inpe.br/radio/observatorio.html |archive-date=July 23, 2010 }}

| Lurigancho-Chosica, Lima Province, Peru

| 50 MHz{{cite document|title=Phase and pattern calibration of the Jicamarca Radio Observatory radar using satellites |publisher= Royal Astronomical Society |date=2014 }}

| 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.{{cite web|title=Jicamarca Radio Observatory |url=http://jro.igp.gob.pe/english/|publisher=JRO |date=2021 |access-date=2021-02-14 }}

| Llano de Chajnantor Observatory, Atacama Desert, Chile

| 30–240 GHz{{cite conference |author=Kohno, K. |title=The Atacama Submillimeter Telescope Experiment |book-title=The Cool Universe: Observing Cosmic Dawn, ASP Conference Series, Vol. 344, Proceedings of the conference held 4–8 October 2004 in Valparaiso, Chile. |bibcode=2005ASPC..344..242K }}

| Array of telescopes located on Cerro Toco and designed to measure the polarization of the CMB.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

|

| 4 m telescope located at Pampa La Bola.

| Eusébio, Brazil

|

| 14.2 m telescope

| 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.

| Llano de Chajnantor Observatory, Atacama Desert, Chile

|

| Located at the Chajnantor plateau.

| Complejo Astronomico El Leoncito (CASLEO), San Juan Province, Argentina

| 212 GHz and 405 GHz

| 1.5 m radome enclosed, single dish Cassegrain antenna, with a focal array (4 beams @ 212 GHz, 2 beams @ 405 GHz) of room temperature receivers.

| La Silla Observatory, Atacama Desert, Chile

|

| 15 m telescope. Decommissioned in 2003{{cite web| url=http://www.eso.org/gallery/v/ESOPIA/LaSilla/esopia00049teles.jpg.html| archive-url=https://archive.today/20120730210903/http://www.eso.org/gallery/v/ESOPIA/LaSilla/esopia00049teles.jpg.html| url-status=dead| archive-date=2012-07-30| title=Swedish-ESO 15m Submillimeter Telescope (SEST)| access-date=2008-08-26}}

| Neuquén Province, Argentina

| S/X/Ka, Delta Dor

| 35 m and 13.5 m Telescopes, Operated by Chinese Deep Space Network (CDSN)

| Malargüe, Argentina

|

| 35 m telescope and deep space antenna, operated by ESTRACK

|Thule Air Base, Greenland

|

|12 metre diameter Cassegrain telescope.

|Adventdalen, Svalbard

|

|Studies of aurorae

| Observatorio del Teide, Canary Islands, Spain

|

| Array of 14 dishes, with two larger source-subtraction dishes. Controlled remotely from UK.

| Arecibo, Puerto Rico

| 8–3,000 MHz

| {{convert|305|m|ft|abbr=on}} Second largest single dish spherical reflector [https://upload.wikimedia.org/wikipedia/commons/thumb/7/7c/Arecibo_Radiotelescopio_SJU_06_2019_7428.jpg/450px-Arecibo_Radiotelescopio_SJU_06_2019_7428.jpg radiotelescope] 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.{{Cite news|date=2020-12-01|title=Puerto Rico: Iconic Arecibo Observatory telescope collapses|language=en-GB|work=BBC News|url=https://www.bbc.co.uk/news/world-us-canada-55147973|access-date=2020-12-02}}

|Mauritius

|

|Mauna Kea Observatory, Hawaii, US

|

|{{convert|10.4|m|ft|abbr=on}} diameter submillimeter wavelength telescope, closed since 2015, due to be dismantled since 2019 to return the land to the natives.

|Mauna Kea Observatory, Hawaii, US

|86, 230, and 345 GHz

|15-meter submillimetre-wavelength telescope operated by the Joint Astronomy Centre

| Mauna Kea Observatory, Hawaii, US

|180–420 GHz

| Operated jointly by the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics of Taiwan.

| Warkworth Radio Observatory, Warkworth, New Zealand

|1.2–21 GHz

| 12 metre fully steerable dish operated by IRASR, Auckland University of Technology{{cite web|title=Radio telescopes – AUT University|url=http://www.irasr.aut.ac.nz/radio-telescope|website=Irasr.aut.ac.nz|access-date=25 October 2015|url-status=dead|archive-url=https://web.archive.org/web/20150929021742/http://www.irasr.aut.ac.nz/radio-telescope|archive-date=29 September 2015}}

| Warkworth Radio Observatory, Warkworth, New Zealand

|6–21 GHz

| 30 metre fully steerable dish operated by IRASR, AUT University

| Signal Hill, Dunedin, New Zealand

|1.575 GHz

| 24-element aperture synthesis open source all-sky radio telescope,{{cite web |url=http://www.github.com/tmolteno/TART |title=TART Source Code |website=Github |access-date=November 9, 2019}} designed and developed by the University of Otago.

| Earth orbit with an apogee altitude of 21,400 km and a perigee altitude of 560 km.

|

| Ceased operations 2005

| Russian spacecraft carrying a radio telescope

|

| Ceased operations 1966

| 10 meter radio telescope in a highly elliptical earth orbit. Launched July 2011.

|

| Ceased operations 2019

| Chinese Earth-Moon L₂ orbiter

|

|

| Chinese base on far side of Moon

|

|

| Chinese lunar orbiter

|

|Nevada, USA

|0.7-2.0 GHz

|An array of 2000 5-meter dishes designed for sky surveys. Expected to start operation in 2026.

|Cambridgeshire, England

|0–11 GHz

| A scientific and educational charitable company currently constructing a Radio Observatory and Ground Station in Cambridgeshire

| 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

| 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.{{cite web|url=http://qttconf.csp.escience.cn/dct/page/70002|archive-url=https://web.archive.org/web/20131224115820/http://qttconf.csp.escience.cn/dct/page/70002|url-status=dead|archive-date=24 December 2013|title=QTT International Advisory Workshop: About QTT|date=24 December 2013|access-date=14 December 2018}}[https://web.archive.org/web/20230405222627/http://qttconf.csp.escience.cn/dct/attach/Y2xiOmNsYjpwZGY6MzMxNDk]

| Carnarvon, South Africa

| L-Band,X-Band,S-Band,UHF

| Additional 128 dishes merged with MeerKAT, expected to be operational in 2022.

|Aguiar, Paraíba, Brazil

|980-1260 MHz

|A crossed-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 the Baryon Acoustic Oscillations through the 21 cm emission line.{{Cite journal |last1=Abdalla |first1=E. |last2=Ferreira |first2=E. G. M. |last3=Landim |first3=R. G. |last4=Costa |first4=A. A. |last5=Fornazier |first5=K. S. F. |last6=Abdalla |first6=F. B. |last7=Barosi |first7=L. |last8=Brito |first8=F. A. |last9=Queiroz |first9=A. R. |last10=Villela |first10=T. |last11=Wang |first11=B. |date=2021-08-19 |title=The BINGO project. I. Baryon acoustic oscillations from integrated neutral gas observations |url=https://www.aanda.org/articles/aa/abs/forth/aa40883-21/aa40883-21.html |journal=Astronomy & Astrophysics |language=en |volume=664 |pages=A14 |arxiv=2107.01633 |doi=10.1051/0004-6361/202140883 |issn=0004-6361 |s2cid=235731903 |doi-access=free}}

|Phthiotis, Greece

|

|32 metre (104 ft.) single dish communication antenna being coverted into a radio telescope by the University of Thessaly and the Hellenic Open University.{{Cite web |title=Wayback Machine |url=https://www.eap.gr/wp-content/uploads/2020/10/%CE%95%CE%BB%CE%BB%CE%B7%CE%BD%CE%B9%CE%BA%CF%8C-%CE%A1%CE%B1%CE%B4%CE%B9%CE%BF%CF%84%CE%B7%CE%BB%CE%B5%CF%83%CE%BA%CE%BF%CF%80%CE%B9%CE%BA%CF%8C-%CE%BA%CE%B1%CE%B9-%CE%A1%CE%B1%CE%B4%CE%B9%CE%BF-%CE%AD%CF%81%CE%B3%CE%B1-%CE%A3%CE%98%CE%95%CE%A4.pdf |archive-url=http://web.archive.org/web/20230126205646/https://www.eap.gr/wp-content/uploads/2020/10/%CE%95%CE%BB%CE%BB%CE%B7%CE%BD%CE%B9%CE%BA%CF%8C-%CE%A1%CE%B1%CE%B4%CE%B9%CE%BF%CF%84%CE%B7%CE%BB%CE%B5%CF%83%CE%BA%CE%BF%CF%80%CE%B9%CE%BA%CF%8C-%CE%BA%CE%B1%CE%B9-%CE%A1%CE%B1%CE%B4%CE%B9%CE%BF-%CE%AD%CF%81%CE%B3%CE%B1-%CE%A3%CE%98%CE%95%CE%A4.pdf |archive-date=2023-01-26 |access-date=2025-02-28 |website=www.eap.gr}}

| China

|

| A 30m aperture sub-millimeter telescope (TSMT) with an active reflector has been proposed in China.[http://144.206.159.178/FT/CONF/16417249/16417327.pdf]{{dead link|date=January 2018|bot=InternetArchiveBot|fix-attempted=yes}}

| Nançay, France

| 10–80 MHz

| The Nancay radio astronomy observatory and associated laboratories are developing the concept of a "Super Station" for extending the LOFAR 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.

| 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.

| 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.

|

| 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.