World Radio Astronomy Observatories
The United States and other countries operate radio astronomy observatories located throughout the world and below is a list of some of the more prominent sites. There are hundreds more radio astronomy sites used by universities and colleges for radio astronomy studies as well as the hundreds of amateur radio astronomers.
| Major Radio Astronomy Facilities | Location | Country |
| Asia Pacific Telescope | Marsfield, New South Wales | Australia |
| Mopra Observatory | Coonabarabran | Australia |
| Parkes Observatory | Parkes | Australia |
| Australia Telescope Compact Array | Narrabri | Australia |
| Australian Long Baseline Array | Parkes-Tidbinbilla | Australia |
| Mount Pleasant Radio Observatory | Hobart, Tasmania | Australia |
| NASA Deep Space Network | Canberra | Australia |
| Very Long Baseline Interferometry | Fortaleza | Brazil |
| Nation River Observatory | Ottawa | Canada |
| Southern Columbia Millimeter Telescope | La Serena | Chile |
| European VLBI Network (JIVE/EVN) Station | Shanghai | China |
| European VLBI Network (JIVE/EVN) Station | Urumgi | China |
| Institut de Radio Astronomie Millimétrique | Plateau de Bure | France |
| Effelsberg Radio Telescope | Effelsberg (Bonn) | Germany |
| Max-Planck Institute for Radio Astronomy | Effelsberg (Bonn) | Germany |
| European VLBI Network (JIVE/EVN) Station | Bologna | Italy |
| European VLBI Network (JIVE/EVN) Station | Noto | Italy |
| European VLBI Network (JIVE/EVN) Station | Medicina | Italy |
| Taed United Kingdom Radio Astronomy Observatory | Taed United Kingdom | Korea |
| Ventspils International Radio Astronomy Center | Ventspils | Latvia |
| Torun Radio Astronomy Observatory | Torun | Poland |
| Hartebeesthoek Radio Astronomy Observatory | Johannesburg | South Africa |
| Institut de Radio Astronomie Millimétrique | Granada | Spain |
| NASA Deep Space Network | Madrid | Spain |
| Onsala Space Observatory (The Swedish National | Onsala | Sweden |
| Kolner Observatory for Submillimeter Astronomy | Gornergrat | Switzerland |
| Westerbork Synthesis Radio Telescope | Westerbork | The Netherlands |
| Cambridge Low-Frequency Synthesis Telescope | Cambridge | United Kingdom |
| Cambridge Ryle Telescope | Cambridge | United Kingdom |
| Cosmic Anisotropy Telescope | Cambridge | United Kingdom |
| European VLBI Network (JIVE/EVN) Station | Jodrell Bank | United Kingdom |
| Mullard Radio Astronomy Observatory | Cambridge | United Kingdom |
| Multi-Element Radio Linked Interferometer Network | Jodrell Bank | United Kingdom |
| Taunton Radio Astronomy Observatory | Somerset | United Kingdom |
| Arecibo Observatory | Arecibo, Puerto Rico | United States |
| Berkeley Illinois Maryland Association-BIMA | Hat Creek, CA | United States |
| Caltech Millimeter Array | Owens Valley, CA | United States |
| Caltech Submillimeter Observatory | Mauna Kea, HI | United States |
| Five College Radio Astronomy Observatory | New Salem, MA | United States |
| Haystack Observatory | Westford, MA | United States |
| James Clerk Maxwell Telescope | Mauna Kea, HI | United States |
| Joint Astronomy Centre | Hilo, HI | United States |
| NASA Deep Space Network | Goldstone, CA | United States |
| NRAO 12-Meter Telescope | Tucson, AZ | United States |
| NRAO Green Bank Telescope | Green Bank, WV | United States |
| NRAO Very Long Array (VLA) | Socorro, NM | United States |
| NRAO Very Long Baseline Array Station | Brewster, WA | United States |
| NRAO Very Long Baseline Array Station | Ft Davis, TX | United States |
| NRAO Very Long Baseline Array Station | Hancock, NH | United States |
| NRAO Very Long Baseline Array Station | Kitt Peak, AZ | United States |
| NRAO Very Long Baseline Array Station | Los Alamos, NM | United States |
| NRAO Very Long Baseline Array Station | Mauna Kea, HI | United States |
| NRAO Very Long Baseline Array Station | North Liberty, IA | United States |
| NRAO Very Long Baseline Array Station | Owens Valley, CA | United States |
| NRAO Very Long Baseline Array Station | Pie Town, NM | United States |
| NRAO Very Long Baseline Array Station | St Croix, VI | United States |
| Ohio State University Radio Observatory | Delaware, OH | United States |
| Owens Valley Radio Observatory | Owens Valley, CA | United States |
| Peach Mountain Radio Observatory | Stinchfield Woods, MI | United States |
| Submillimeter Telescope Observatory | Emerald Peak, AZ | United States |
Since its beginning, radio astronomy has contributed much to the science of astronomy and has had numerous innovations that have benefitted radiocommunications and mankind in general. The tables below list some of the advances and contributions to medical, industrial, defense, and environmental applications.(1)
| Astronomical Technique or Device | Medical Uses |
| • 3-D image reconstruction from one- and
two-dimensional images |
• Imaging for CAT scans
• Magnetic resonance imaging • Positron emission tomography |
| • Microwave receivers | • Scans for breast cancer |
| • Image-processing software (IRAF and AIPS) developed by NRAO, NOAA, and NASA | • Cardiac angiography
• Monitoring neutron activity in brain |
| • Positive pressure clean rooms for assembly of space instruments | • Cleaner hospital operating rooms |
| • Detection of faint x-ray sources | • Portable x-ray scanners (Lixiscope) for neonatology and third world clinics |
| Astronomical Technique or Device | Industrial Uses |
| • Image-processing software (AIPS, IRAF) | • General Motors Co. study of automobile crashes; Boeing Co. tests of aircraft hardware |
| • Holographic methods for testing figures of radio telescopes | • Testing communications antennas |
| • Development of low-noise receivers | • Components for communications industry |
| • FORTH computer language developed by NRAO for
control of radio telescopes |
• 20 vendors supply FORTH for applications including analysis of auto engines in 20,000 garages, quality control for films at Kodak, 50,000 hand-held computers used by express mail firm. |
| • Gold sensitization of photographic plates | • Development of Tri-X and 400-ASA films by Kodak |
| • Infrared-sensitive films for spectroscopy | • Aerial reconnaissance and Earth resources mapping |
| • X-ray detectors for NASA telescopes
• Gas Chromatographs to search for life on Mars |
• Baggage scanners at airports |
| Astronomical Technique or Device | Defense Uses |
| • Stellar observations and model atmospheres
• Infrared all-sky survey by NASA'S IRAS satellite. |
• Discrimination of celestial objects from rocket plumes, satellites, and warheads |
| • Detectors for gamma-ray and x-ray astronomy | • Vela satellite monitors for nuclear explosions |
| • Positions of quasar and stars | • Precision navigation for civil and military purposes |
| Astronomical Technique or Device | Environmental Uses |
| • Millimeter wave spectroscopy | • Study of ozone depletion |
| • Models of planetary atmospheres | • Global change modeling |
| • Study of sunspots and solar flares in sun and stars | • Short- and long-term predictions of terrestrial effects |
| • Models of astrophysical shocks | • Study of terrestrial storms |
| • Precision measurement of quasars | • Geodesy and study of tectonic drift |
| • Composite materials for orbiting infrared telescope | • Design of solar collectors |
| • Theory of cosmic rays, solar flares, and stellar fusion | • Design of fusion reactors |
Preferred Frequency Bands
for Radio Astronomical Measurements
The source of the following three tables was Recommendation 314-8, ITU-R Recommendations, 1994 RA Series, Radioastronomy. Further, these revised lists of frequencies of the astrophysically most important spectral lines were approved by the General Assembly of the IAU, 1991.
| TABLE C-1.
Radio Frequency Lines of the Greatest Importance to Radio Astronomy at Frequencies Below 275 GHz | |||||
| Substance | Rest
Frequency |
Suggested Minimum
Band |
Notes (1) | ||
| Deuterium (DI) | 327.384 | MHz | 327.0 - 327.7 | MHz | 2,3 |
| Hydrogen (HI) | 1420.406 | MHz | 1370.0 - 1427.0 | MHz | |
| Hydroxyl radical (OH) | 1612.231 | MHz | 1606.8 - 1613.8 | MHz | 4 |
| Hydroxyl radical (OH) | 1665.402 | MHz | 1659.8 - 1667.1 | MHz | 4 |
| Hydroxyl radical (OH) | 1667.359 | MHz | 1661.8 - 1669.0 | MHz | 4 |
| Hydroxyl radical (OH) | 1720.530 | MHz | 1714.8 - 1722.2 | MHz | 3, 4 |
| Methyladyne (CH) | 3263.794 | MHz | 3252.9 - 3267.1 | MHz | 3, 4 |
| Methyladyne (CH) | 3335.481 | MHz | 3324.4 - 3338.8 | MHz | 3, 4 |
| Methyladyne (CH) | 3349.193 | MHz | 3338.0 - 3352.5 | MHz | 3, 4 |
| Formaldehyde (H2CO) | 4829.660 | MHz | 4813.6 - 4834.5 | MHz | 3, 4 |
| Methanol (CH3OH) | 6668.518 | MHz | 6661.8 - 6675.2 | MHz | 3, 6 |
| Helium (3He+) | 8665.650 | MHz | 8657.0 - 8674.3 | MHz | 3, 6 |
| Methanol (CH3OH) | 12.178 | GHz | 12.17 - 12.19 | GHz | 3, 6 |
| Formaldehyde (H2CO) | 14.488 | GHz | 14.44 - 14.50 | GHz | 3, 4 |
| Cyclopropenylidene (C3H2) | 18.343 | GHz | 18.28 - 18.36 | GHz | 3, 4, 6 |
| Water vapor (H2O) | 22.235 | GHz | 22.16 - 22.26 | GHz | 3, 4 |
| Ammonia (NH3) | 23.694 | GHz | 23.61 - 23.71 | GHz | 4 |
| Ammonia (NH3) | 23.723 | GHz | 23.64 - 23.74 | GHz | 4 |
| Ammonia (NH3) | 23.870 | GHz | 23.79 - 23.89 | GHz | 4 |
| Silicon monoxide (SiO) | 42.821 | GHz | 42.77 - 42.86 | GHz | |
| Silicon monoxide (SiO) | 43.122 | GHz | 43.07 - 43.17 | GHz | |
| Carbon monosulphide (CS) | 48.991 | GHz | 48.94 - 49.04 | GHz | |
| Deuterated formylium (DCO+) | 72.039 | GHz | 71.96 - 72.11 | GHz | 3 |
| Silicon monoxide (SiO) | 86.243 | GHz | 86.16 - 86.33 | GHz | |
| Formylium (H13CO+) | 86.754 | GHz | 86.66 - 86.84 | GHz | |
| Silicon monoxide (SiO) | 86.847 | GHz | 86.67 - 86.93 | GHz | |
| Ethynyl radical (C2H) | 87.3 | GHz | 87.21 - 87.39 | GHz | 5 |
| Hydrogen cyanide (HCN) | 88.632 | GHz | 88.34 - 88.72 | GHz | 4 |
| Formylium (HCO+) | 89.189 | GHz | 88.89 - 89.28 | GHz | 4 |
| Hydrogen isocyanide (HNC) | 90.664 | GHz | 90.57 - 90.76 | GHz | |
| Diazenylium (N2H+) | 93.174 | GHz | 93.07 - 93.27 | GHz | |
| Carbon monosulphide (CS) | 97.981 | GHz | 97.65 - 98.08 | GHz | 4 |
| Carbon monoxide (C18O) | 109.782 | GHz | 109.67 - 109.89 | GHz | |
| Carbon monoxide (13CO) | 110.201 | GHz | 109.83 - 110.31 | GHz | 4 |
| Carbon monoxide (C17O) | 112.359 | GHz | 112.25 - 112.47 | GHz | 6 |
| Carbon monoxide (CO) | 115.271 | GHz | 114.88 - 115.39 | GHz | 4 |
| Formaldehyde (H213CO) | 137.450 | GHz | 137.31 - 137.59 | GHz | 3, 6 |
| Formaldehyde (H2CO) | 140.840 | GHz | 140.69 - 140.98 | GHz | |
| Carbon monosulphide (CS) | 146.969 | GHz | 146.82 - 147.12 | GHz | |
| Water vapor (H2O) | 183.310 | GHz | 183.12 - 182.50 | GHz | |
| Carbon monoxide (C18O) | 219.560 | GHz | 219.34 - 219.78 | GHz | |
| Carbon monoxide (13CO) | 220.399 | GHz | 219.67 - 220.62 | GHz | 4 |
| Carbon monoxide (CO) | 230.538 | GHz | 229.77 - 230.77 | GHz | 4 |
| Carbon monosulphide (CS) | 244.953 | GHz | 244.72 - 245.20 | GHz | 6 |
| Hydrogen cyanide (HCN) | 265.886 | GHz | 265.62 - 266.15 | GHz | |
| Formylium (HCO+) | 267.557 | GHz | 267.29 - 267.83 | GHz | |
| Hydrogen isocyanide (HNC) | 271.981 | GHz | 271.71 - 272.25 | GHz | |
| Notes:
1. If Notes 4 or Note 2 are not listed, the band limits are the Doppler-shifted frequencies corresponding to radial velocities of ± 300 km/s (consistent with line radiation occurring in our Galaxy). 2. An extension to lower frequency of the allocation of 1400-1427 MHz is required to allow for the higher Doppler shifts for HI observed in distant galaxies. 3. The current international allocation is not primary and/or does not meet bandwidth requirements. See the Radio Regulation for more detailed information. 4. Because these line frequencies are also being used for observing other galaxies, the listed bandwidths include Doppler shifts corresponding to radical velocities of up to 1,000 km/s. It should be noted that HF had been observed at frequencies redshifted to 500 MHz, while some lines of the most abundant molecules have been detected in galaxies with velocities up to 50,000 km/s, corresponding to a frequency reduction of up to 17%. 5. There are six closely spaced lines associated with this molecule at this frequency. The listed band is wide enough to permit observations of all six lines. 6. This line frequency is not mentioned in Article 8 of the Radio Regulations. | |||||
| TABLE C-2.
Radio Frequency Lines of the Greatest Importance to Radio Astronomy at Frequencies Between 275 and 811 GHz (not allocated in the Radio Regulations) | ||
| Substance | Rest Frequency (GHz) | Suggested Minimum Band (GHz) |
| Diazenylium (N2H+) | 279.511 | 279.23 - 279.79 |
| Carbon monoxide (C18O) | 329.330 | 329.00 - 329.66 |
| Carbon monoxide (13CO) | 330.587 | 330.25 - 330.92 |
| Carbon monosulphide (CS) | 342.883 | 342.54 - 343.23 |
| Carbon monoxide (CO) | 345.796 | 345.45 - 346.14 |
| Hydrogen cyanide (HNC) | 354.484 | 354.13 - 354.84 |
| Formylium (HCO+) | 356.734 | 356.37 - 357.09 |
| Diazenylium (N2H+) | 372.672 | 372.30 - 373.05 |
| Water vapor (H2O) | 380.197 | 379.81 - 380.58 |
| Carbon monoxide (C18O) | 439.088 | 438.64 - 439.53 |
| Carbon monoxide (13CO) | 440.765 | 440.32 - 441.21 |
| Carbon monoxide (CO) | 461.041 | 460.57 - 461.51 |
| Heavy water (HDO) | 464.925 | 464.46 - 465.39 |
| Carbon (CI) | 492.162 | 491.66 - 492.66 |
| Water vapor (H218O) | 547.676 | 547.13 - 548.22 |
| Water vapor (H2O) | 556.936 | 556.37 - 557.50 |
| Ammonia (15NH3) | 572.113 | 571.54 - 572.69 |
| Ammonia (NH3) | 572.498 | 571.92 - 573.07 |
| Carbon monoxide (CO) | 691.473 | 690.78 - 692.17 |
| Hydrogen isocyanide (HNC) | 797.433 | 796.64 - 798.23 |
| Formylium (HCO+) | 802.653 | 801.85 - 803.85 |
| Carbon monoxide (CO) | 806.652 | 805.85 - 807.46 |
| Carbon (CI) | 809.350 | 808.54 - 810.16 |
| TABLE C-3.
Frequency Bands Allocated to the Radio Astronomy Service That Are Preferred for Continuum Observations (Secondary allocations are contained within brackets) | |||
| Frequency Band
(MHz) |
Bandwidth
(%) |
Frequency Band
(GHz) |
Bandwidth
(%) |
| 13.360-13.410 | 0.37 | 10.6-10.7 | 0.94 |
| 25.550-25.670 | 0.49 | 15.35-15.4 | 0.33 |
| [37.5-38.25] | [1.98] | 22.21-22.50 | 1.30 |
| 73-74.6 [1] | 2.17 | 23.6-24.0 | 1.68 |
| 150.05-153 [2] | 1.95 | 31.3-31.8 | 1.58 |
| 322-328.6 | 2.03 | 42.5-43.5 | 2.33 |
| 406.1-410 | 0.96 | 86-92 | 6.74 |
| 608-614 [3] | 0.98 | 105-116 | 9.95 |
| 1400-1427 | 1.91 | 164-168 | 2.41 |
| 1660-1670 | 0.60 | 217-231 | 6.25 |
| 2690-2700 [2655-2690 ] | 0.37 [1.31] | 265-275 | 3.70 |
| 4990-5000 [4800-4990 ] | 0.20 [3.88] | ||
| Notes:
(1) Allocation (primary) in Region 2, protection recommended in Regions 1 and 3. (2) Allocation (primary) in Region 1, Australia, and India. (3) Allocation (primary) in Region 2, China, and India. | |||
AM Amplitude Modulation
am Attometer (10-18 meter)
CAT Computer-aided Tomographic
cm Centimeter (10-2 meter)
CRAF Committee on Radio Astronomy Frequencies
DOD Department of Defense
EHF Extra High Frequency
EPIRB Emergency Position Indicating Radiobeacon
FAA Federal Aviation Administration
FCC Federal Communications Commission
FM Frequency Modulation
fm Femtometer (10-15 meter)
FN Footnote
GHz Gigahertz (109 Hertz)
GLONASS Global Navigation Satellite System (Russian Federation System)
GPO Government Printing Office
GPS Global Positioning System
HF High Frequency
IAU International Astronomical Union
ICAO International Civil Aviation Organization
IRAC Interdepartment Radio Advisory Committee
ITU International Telecommunication Union
kHz Kilohertz (103 Hertz)
km Kilometer
m Meter
MHz Megahertz (106 Hertz)
µm Micrometer (10-6 meter)
mm Millimeter (10-3 meter)
MRI Magnetic Resonance Imaging
NASA National Aeronautics and Space Administration
nm Nanometer (10-9 meter)
NOAA National Oceanic and Atmospheric Administration
NRAO National Radio Astronomy Observatory
NSF National Science Foundation
NTIA National Telecommunications and Information Administration
OH Hydroxyl
(OR) Off-route
PCS Personal Communications Service
pm Picometer (10-12 meter)
(R) Route
SARSAT Search and Rescue Satellite-aided Tracking
SHF Super High Frequency
SPAC Spectrum Planning and Policy Advisory Committee
THz Terahertz (1012Hertz)
UHF Ultra High Frequency
VHF Very High Frequency
VLA Very Long Array
VLBI Very Long Baseline Interferometry
WARC World Administrative Radio Conference
WRC World Radiocommunication Conference (formerly WARC)
1. See National Research Council, supra note 13, at 130-133.
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