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• telescope : Frederick C. Gillett Gemini North 8.1-m Telescope
  The Gemini Observatory consists of twin 8.1-meter diameter optical/infrared telescopes located on two of the best observing sites on the planet. From their locations on mountains in Hawai'i and Chile, Gemini Observatory's telescopes can collectively access the entire sky. The Frederick C. Gillett Gemini North telescope is located on Hawaii's Mauna Kea as part of the international community of observatories built to take advantage of the superb atmospheric conditions on this long dormant volcano which rises about 4,214 meters (13,824 feet) into the dry, stable air of the Pacific. Primary Mirror: Diameter: 8.1 meters/26.58 feet/319 inches Mass: 22.22 metric tonnes/24.5 U.S. tons Composition: Corning Ultra-Low Expansion (ULE) Glass Surface Accuracy: 15.6 nm RMS (Between 1/1000 - 1/10,000 thickness of human hair)`
• telescope : Copernico 1.82m Telescope
  The Copernico 1.82m Telescope is a 1.82 m telescope located at 45.843400, 11.571400 at the Asiago Astrophysical Observatory. The Asiago 1.82m telescope, inaugurated in 1973 and dedicated to N. Copernicus, is a classic Cassegrain reflector. It is the main observing facility at the observing site of Cima Ekar (1350m) of the Asiago Astrophysical Observatory.
• telescope : El Leoncito Astronomical Complex 2.15-m Boller and Chivens Reflector
  The 2.15-m Boller & Chivens reflector is a 2.15 m telescope located at -31.799166, 290.699997 at the El Leoncito Astronomical Complex. Operational 02/1986+
• telescope : MDM Observatory 2.4-m Hiltner Ritchey-Chretien Equatorial Reflector
  The Hiltner 2.4-meter Telescope is an optical telescope located at the MDM Observatory on Kitt Peak, Arizona. Operational since 1986, it is a Ritchey-Chrétien reflector with a primary mirror made of aluminum-coated Cer-Vit. The telescope is equipped with multiple focal points, including f/7.5 and f/13.5 Cassegrain configurations, allowing for a variety of astronomical observations. It is primarily used for galactic surveys and has contributed to significant discoveries, such as the detection of the transient event PS1-13cbe in the galaxy SDSS J222153.87+003054.2.
• telescope : DSS-13 26-m Radio Telescope
  This fully steerable telescope was a research and development radio/radar antenna that was part of the NASA Deep Space Network. It was first operational in 1962 with a 26-m aperture and was named "Venus Station" to commemorate the first radar detection of Venus by radar facilities at Goldstone in 1961. The 26-m antenna was decommissioned in 1991. Its cordinates are not known. A 34-m beam waveguide (BWG) antenna was completed in 1991 at the same general location. It was given the DSS-13 identifier and was used to contnue research and development work at higher frequencies.
• telescope : DSS-13 34-m Radio Telescope
  This fully steerable telescope is a research and development radio/radar antenna that is part of the NASA Deep Space Network. It was first operational in 1962 with a 26-m aperture and was named "Venus Station" to commemorate the first radar detection of Venus by radar facilities at Goldstone in 1961; the 26-m antenna was decommissioned in 1991. A 34-m beam waveguide (BWG) antenna was completed that year to facilitate development work at higher frequencies. DSS-13 has been used occasionally in conjunction with the Goldstone Solar System Radar for radar interferometry. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005) and apply to the 34-m BWG antenna as used since 1991.
• telescope : DSS-14 64-m Radio Telescope
  This fully steerable telescope is a parabolic radio/radar antenna that is part of the NASA Deep Space Network (DSN). DSS-14 was first operational in 1964 with a 64-m aperture, supporting the Mariner 4 flyby of Mars; as a result, it was subsequently known as "Mars Station". Its aperture was extended to 70-m in 1988 to support the Voyager 2 encounter with Neptune. The 64-m antenna could receive at frequencies between about 1.6 and 8.6 GHz in left-circular polarization (LCP); over 2.0-8.6 GHz it could receive simultaneously in both LCP and right-circular polarization (RCP). It could transmit up to 20 kW at selected frequencies in the 2-8 GHz range. DSS-14 was used occasionally as part of the Goldstone Solar System Radar, which has more powerful transmitters. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005).
• telescope : DSS-14 70-m Radio Telescope
  This fully steerable telescope is a parabolic radio/radar antenna that is part of the NASA Deep Space Network (DSN). DSS-14 was first operational in 1964 with a 64-m aperture, supporting the Mariner 4 flyby of Mars; as a result, it was subsequently known as "Mars Station". Its aperture was extended to 70-m in 1988 to support the Voyager 2 encounter with Neptune. The antenna can receive at frequencies between about 1.6 and 8.6 GHz in left-circular polarization (LCP); over 2.0-8.6 GHz it can receive simultaneously in both LCP and right-circular polarization (RCP). It can transmit up to 20 kW at selected frequencies in the 2-8 GHz range. DSS-14 is used occasionally as part of the Goldstone Solar System Radar, which has more powerful transmitters. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005).
• telescope : DSS-15 34-m Radio Telescope
  This fully steerable telescope iss a dual-shaped reflector radio antenna that was part of the NASA Deep Space Network. It was part of the Goldstone Deep Space Communications Complex (GDSCC) near Barstow, California (USA). DSS 15 was first operational in the mid-1980s with a 34-m aperture; it was decommissioned in May 2018. When operational, the antenna could receive at frequencies in the range 2.0-8.6 GHz in right- or left-circular polarization (but not simultaneously). It could transmit 50-250 W at 2.1 GHz or up to 20 kW at 7.1 GHz. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). DSS-15 was sometimes known as "Uranus Station". GDSCC is managed by the Jet Propulsion Laboratory (JPL) in Pasadena, CA.
• telescope : DSS-16 Radio Telescope
  This 26-meter (85-ft.) diameter antenna was originally designed as part of the Manned Space Flight Network (MSFN), managed by Goddard Space Flight Center. At the completion of the Apollo missions, DSS-16 was designated a part of the Satellite Tracking and Data Network (STDN) and used for tracking Earth orbiting satellites and for initial acquisition of any spacecraft immediately after launch. It partnered with DSS-46 (near Canberra, Australia) and DSS-66 (near Madrid, Spain) in a 26-m subnet for this purpose. In the 1990s it provided communications with NASA's Space Shuttle. DSS-16 could transmit 50-2000 W at 2.1 GHz (S-band). It could receive right- and left-circularly polarized signals simultaneously at both 2.3 GHz and 8.4 GHz; its receiver could combine the signals to obtain a rotatable linear polization. The antenna was completed in 1966 and remained part of NASA's tracking networks until the mid-2000s.
• telescope : DSS-23 Radio Telescope
  DSS-23 is a 34-m beam waveguide (BWG) antenna expected to become operational in 2024. It will transmit 20 kW at 7.1 GHz and receive right- and left-polarized signals at 8.4 and 32 GHz. No coordinates are available for the antenna at this time.
• telescope : DSS-24 34-m Radio Telescope
  DSS-24 is one of three beam waveguide (BWG) antennas constructed between 1992 and 1996 in a cluster at "Apollo Valley" within the Goldstone Deep Space Communications Complex (GDSCC). These antennas were the first DSN operational antennas to utilize the BWG design that moves environmentally sensitive electronic equipment into an underground pedestal, instead of a centrally mounted feed cone structure. The use of the underground pedestal also allows for easier repair, maintenance, and upgrades. DSS-24 operates at both S- and X-band (2 and 8 GHz, respectively) with 20 kW transmitters on both bands. It can receive right- or left-circular polarization (RCP or LCP) at S-band and simultaneous RCP and LCP at X-band. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005).
• telescope : DSS-25 34-m Radio Telescope
  DSS-25 is one of three beam waveguide (BWG) antennas constructed between 1992 and 1996 in a cluster at "Apollo Valley" within the Goldstone Deep Space Communications Complex (GDSCC) . These antennas were the first DSN operational antennas to utilize the BWG design that moves environmentally sensitive electronic equipment into an underground pedestal instead of a centrally mounted feed cone structure. The use of the underground pedestal also allows for easier repair, maintenance, and upgrades. DSS-25 operates at both X-band and Ka-band (8 and 34 GHz, respectively) with a 20 kw transmitter at X-band and a 300 W transmitter at Ka-band. DSS-25 can receive right- and left-circular polarization (RCP and LCP, respectively) simultaneously on both bands. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005).
• telescope : DSS-26 34-m Radio Telescope
  DSS-26 is one of three beam waveguide (BWG) antennas constructed between 1992 and 1996 in a cluster at "Apollo Valley" within the Goldstone Deep Space Communications Complex (GDSCC) . These antennas were the first DSN operational antennas to utilize the BWG design that moves environmentally sensitive electronic equipment into an underground pedestal instead of a centrally mounted feed cone structure. The use of the underground pedestal also allows for easier repair, maintenance and upgrades. DSS-26 operates at S-, X-, and Ka-band (2, 8, and 34 GHz, respectively). On S-band its transmitter radiates 250 W; it can receive either right- or left-circular polarization (RCP or LCP, respectively). On X-band, its transmitter is rated for 20 kW; it can receive RCP and LCP simultaneously. At Ka-band it can receive RCP and LCP simultaneously but not transmit. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005).
• telescope : DSS-27 34-m Radio Telescope
  DSS-27 is one of two high-speed beam waveguide (HSB) antennas constructed by the Jet Propulsion Laboratory at the Goldstone Deep Space Communications Complex (GDSCC) for the U.S. Army; they were transferred to NASA in 1994. The beam waveguide (BWG) design moves environmentally sensitive electronic equipment from a cone at the reflector focus into a pedestal. The radio signal is guided from the subreflector through a hole in the surface of the dish to the receiving equipment in the pedestal via a system of reflecting mirrors inside a large tube. The reverse path allows transmission. The BWG design reduces weight on the reflecting surface, provides insulation of electronics from environmental factors including dish movement, and simplifies maintenance. The HSB antenna differs from other BWG antennas in that the pedestal room is above ground level (rather than underground), the optics design is different, and the subreflector does not focus automatically for the purpose of maintaining gain as the elevation angle of the antenna changes. The HSB antenna has higher tracking rates than do other BWG antennas; thus, it is an appropriate antenna to use when tracking Earth-orbiting satellites. DSS-27 was decommissioned in the mid-2010s. When operational it could transmit 50-200 W at 2.1 GHz and receive right- or left-circularly polarized signals at 2.2 GHz.
• telescope : McGraw-Hill Observatory 1.3-m Tinsley Cassegrain/Coude Reflector
  The 1.3-meter Tinsley Cassegrain/Coude reflector is an optical telescope located at the McGraw-Hill Observatory on Kitt Peak, Arizona. Operational since May 1975, it was originally part of the University of Michigan Radio Astronomy Observatory before being transferred to the observatory. This telescope has been utilized for various astronomical observations, including planetary studies and asteroid research. Its Cassegrain and Coudé focal configurations allow for versatile instrumentation, making it a valuable asset for both research and educational purposes.
• telescope : Orion Astroview 120ST EQ
  The Orion Astroview 120ST EQ is a 12 cm telescope located at 32.155000, 248.918000 at the Goodricke-Pigott Observatory. Orion Astroview 120ST EQ 120 mm aperture f/5 refractor, mounted on a Vixen "Great Polaris Deluxe" high precision equatorial mount and tripod instead of the standard mount. The mounting was equipped with the Vixen "Sky Sensor 2000" computer hand paddle and motor drive system which provided tracking and Go-To capability.
• telescope : Observatory of Haute-Provence 1.20-m Newtonian Reflector
  The 1.20-m Newtonian reflector is a 1.20 m telescope located at 43.931751, 5.715694 at the Observatory of Haute-Provence. Operational 1943+; from Paris Obs.
• telescope : Observatorio Astronomico Nacional 1.5 m Telescope
  The 1.5 m is a 1.5 m telescope located at 31.577700, 115.466600 at the National Astronomical Observatory-Ensenada. The Instituto de Astronomia at Ensenada, Mexico, operates the 1.5m, f/13.5 Ritchey-Chretien reflector telescope at the Observatorio Astronomico Nacional/San Pedro Martir facility located on the summit of the San Pedro Martir Sierra on the Baja California peninsula of Mexico. The telescope was installed in 1970. The 1.5m telescope is located at: Longitude : 115.466667 degrees West (-115deg 28' 00'') Latitude : 31.045278 degrees North ( +31deg 02' 43'') Altitude : 2790 meters This information is provided at the Observatorio Astronomico Nacional website: http://www.astrossp.unam.mx/indexspm.html
• telescope : DSS 11 Radio Telescope
  Pioneer Station (DSS-11), a 26 meter polar mounted antenna, was the first deep space antenna to be constructed at Goldstone. Completed in December 1958, in time to support the Pioneer 3 mission, DSS-11 became the prototype antenna for the Deep Space Network (DSN) and went on to track a variety of NASA spacecraft including all Pioneers, the Echo balloons, and the Ranger, Lunar Orbiter, Surveyor, Apollo, Helios, Mariner, Viking, and Voyager spacecraft. A Manned Space Flight wing was built at the Pioneer site to support the manned space flights of the Apollo program. DSS-11 was officially mothballed in 1981 and was declared a National Historic Monument as the first deep space antenna in the DSN in 1985. Antenna coordinates are approximate; they were interpolated from coordinates for DSS-13 and DSS-14 in Table 5 of module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005) using the map at https://www.gdscc.nasa.gov/?page_id=37
• telescope : 10-m Keck I Ritchey-Chretien Altazimuth Reflector
  The 10-m Keck I Ritchey-Chretien altazimuth reflector is a 10 m telescope located at 19.825945, 204.525284 at the W.M. Keck Observatory. The Keck I telescope began science operations in May, 1993. It was built through the W. M. Keck Foundation and is operated by the California Association for Research in Astronomy which includes the University of California, the California Institute of Technology and the National Aeronautics and Space Administration. The Keck I is located at the W. M. Keck Observatory near the summit of Mauna Kea, Hawaii. The geodetic coordinates of the telescope are: Longitude : 155d 28.4' W Latitude : +19d 49.6' N Altitude: : 4124m Mean seeing : about 0.5 arcseconds full-width-half-max in the K-band The overview and location given here are reproduced from the W. M. Keck Observatory web site, http://www2.keck.hawaii.edu/. Telescope Properties -------------------- The primary mirror comprises 36 hexagonal segments. Each segment is 1.8 meters, measured across the corners. The maximum diameter of the primary mirror is 10.5 meters, and its focal length is 17.5 meters. The telescope has 2 secondary mirrors. The f/15 secondary mirror forms a Richey Chretien system with the primary mirror. It can be used directly with an instrument mounted at the rear of the support structure for the primary mirror or with a flat tertiary mirror for a bent Cassegrain or Nasmyth focus. The f/25 secondary mirror is used with the infrared instruments at Keck I. The gold-plated mirror has a central hole to reduce the reflection of radiation to the detector from beyond the edge of the primary mirror or from the central obstruction for chop angles up to +/-150 arcseconds. A chopping mechanism resides behind this secondary mirror and does not obstruct the detector. As the chopping mechanism tilts, the image moves on the detector. This provides a way to rapidly center a target on the detector, then chop to a nearby part of sky without moving the telescope. The Keck Observatory website provides a tutorial for the chopping mechanism, http://www2.keck.hawaii.edu/inst/tools/chp/Chopping.html. The optical features of the f/15 and f/25 secondary mirror are: f/15 f/25 ----- ------ Focal length (m) : 149.6 249.7 Scale (mm/arcsec) : 0.725 1.211 Field diameter (arcmin) : 20 10 Field diameter (mm) : 870 727 Radius of curvature* (m) : 2.14 0.82 The telescope properties given here are reproduced from the Keck Telescope and Facility Instrument Guide, available at http://www2.keck.hawaii.edu/observing/kecktelgde/ktelinstupdate.pdf.
• telescope : 10-m Keck II Ritchey-Chretien Altazimuth Reflector
  The 10-m Keck II Ritchey-Chretien altazimuth reflector is a 10 m telescope located at 19.826557, 204.525772 at the W.M. Keck Observatory. Operational 04/1996+; 36 1.8-m mirrors
• telescope : Very Large Telescope (VLT) Unit Telescope 4 (UT4) Yepun, 8.2-m Telescope
  Unit Telescope 4 (Yepun) of the Very Large Telescope (VLT) at ESO's Paranal Observatory, Chile. The telescope is one of four 8.2-m Ritchey-Chretien Cassegrain telescopes with a 22-tonne Zerdour primary mirror of 14.4 m focal length, and a 1.1-m lightweight beryllium secondary mirror. The unit telescope has alt-azimuth mount. In such a mount the telescope tube moves around a horizontal axis called elevation axis. The two bearings which support the tube are mounted on a fork rotating around a vertical axis, called azimuth axis, thus allowing for pointing over the entire sky. The telescope tube itself consists of a steel structure supporting at the bottom the primary mirror (M1) in its cell, and at the top the M2 Unit by means of metallic beams called "spiders". The Very Large Telescope uses active optics.The optical quality of the image is continually monitored by an image analyser using a reference star and the contributions of the various optical aberrations (defocus, astigmatism, coma, etc.) are computed. To achieve the best optical quality, discrete correction commands are given to the primary mirror support system, controlling the shape of the thin flexible M1,and to the M2 Unit, which controls the position of the M2 mirror along 5 degrees of freedom, namely one for focusing,two for centering, and two for pointing. The M2 mirror itself is configured as a rigid lightweight convex hyperboloid. Information from the ESO telescope website: http://www.eso.org/sci/facilities/paranal/telescopes/ut.html
• telescope : Kitt Peak 1.3-m Boller and Chivens Cassegrain Reflector
  The 1.3-m Boller & Chivens Cassegrain reflector is a 1.3 m telescope located at 31.959583, 248.402283 at the Kitt Peak National Observatory. c.1965+
• telescope : Kitt Peak 2.13-m Corning Cassegrain/Coude reflector
  The 2.13-m Corning Cassegrain/Coude reflector is a 2.13 m telescope located at 31.958113, 248.402344 at the Kitt Peak National Observatory. Operational 09/1964+
• telescope : Kitt Peak 4-m Mayall Ritchey-Chretien equatorial reflector
  The 4-m Mayall Ritchey-Chretien equatorial reflector is a 4 m telescope located at 31.963972, 248.400658 at the Kitt Peak National Observatory. Operational 02/1973+
• telescope : Kuiper Airborne 0.91m Telescope
  Cassegrain reflector with a 36-inch (91.5 cm) aperture, designed primarily for observations in the 1 to 500 μm spectral range.
• telescope : Irenee du Pont 2.5m Telescope
  The Irénée du Pont 2.5-meter Telescope, located at Las Campanas Observatory in Chile, has been operational since 1977 and is managed by the Carnegie Institution for Science. As a Ritchey-Chrétien reflector, it supports a wide range of astronomical research, including stellar spectroscopy and supernova observations. Notably, it serves as the southern hemisphere platform for the APOGEE-2 survey, part of the Sloan Digital Sky Survey, enabling detailed studies of the Milky Way's structure and evolution.
• telescope : Walter Baade Telescope at Las Campanas Observatory
  The Walter Baade telescope is one of a twin pair (with the Landon T. Clay) located on Cerro Manqui at Las Campanas Observatory. The primary mirror is an f/1.25 parabaloid with a honeycomb internal structure to reduce weight. The telescope optics include active controls, including correction of low-order aberrations by controlling the figure of the primary mirror.
• telescope : Landon T. Clay Telescope at Las Campanas Observatory
  The Landon T. Clay telescope is one of a twin pair (with the Walter Baade) located on Cerro Manqui at Las Campanas Observatory. The primary mirror is an f/1.25 parabaloid with a honeycomb internal structure to reduce weight. The telescope optics include active controls, including correction of low-order aberrations by controlling the figure of the primary mirror.
• telescope : Swope 1.0m Telescope
  The Swope 1.0-meter Telescope, located at Las Campanas Observatory in Chile, has been operational since 1971 and is named after astronomer Henrietta Hill Swope. As the observatory's first telescope, it has played a pivotal role in various astronomical studies, including the initial phase of the Optical Gravitational Lensing Experiment (OGLE) in 1992 . The telescope has also been instrumental in projects like the Cluster AgeS Experiment (CASE), which investigates the ages and distances of globular clusters through observations of eclipsing binaries . In 2017, the Swope Telescope contributed to the discovery of SSS17a, the optical counterpart to the gravitational wave event GW170817.
• telescope : Las Cumbres Global Telescope Network - 0.4m Telescopes
  The 40cm telescopes of the Las Cumbres global network are built to be identical. They are Meade 16-inch (40cm), 3-element optics telescopes mounted in LCO equatorial C-ring mountings. Users should consult the data product documentation to determine which telescope was used to record any specific observation when that information is needed.
• telescope : DSS-12 26-m Radio Telescope
  Echo Station (DSS-12) is currently the administrative center for the Goldstone Deep Space Communications Complex (GDSCC). Built in 1959 with a 26-m aperture, DSS-12 is named for early experiments performed with the passive balloon satellite, Echo 1. The antenna is polar mounted, was upgraded to a 34-m aperture in 1979, and was capable of simultaneously operating at both S- and X-band frequencies. For 37 years, DSS-12 supported many spacecraft including the early Ranger and Surveyor missions to the Moon, deep space missions such as Pioneer and Voyager, and high Earth orbiting spacecraft. Antenna coordinates are approximate; they were interpolated from coordinates for DSS-13 and DSS-14 in Table 5 of module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005) using the map at https://www.gdscc.nasa.gov/?page_id=37
• telescope : Las Cumbres Global Telescope Network - 2m Telescopes
  The 2m telescopes of the Las Cumbres global network are built to be identical. They are Altitude-Azimuth mounted Ritchey-Chretian Cassegrain telescopes. Users should consult the data product documentation to determine which telescope was used to record any specific observation when that information is needed.
• telescope : DSS-12 34-m Radio Telescope
  Echo Station (DSS-12) is currently the administrative center for the Goldstone Deep Space Communications Complex (GDSCC). Built in 1959 with a 26-m aperture, the station is named for early experiments performed with the passive balloon satellite, Echo 1. The antenna is polar mounted, was upgraded to a 34-m aperture in 1979, and was capable of simultaneously operating at both S- and X-band frequencies. For 37 years, DSS-12 supported many spacecraft including the early Ranger and Surveyor missions to the Moon, deep space missions such as Pioneer and Voyager, and high Earth orbiting spacecraft. In 1996 the antenna was removed from DSN operations and used in an educational outreach project between NASA's Jet Propulsion Laboratory and the Lewis Center for Educational Research. In 2012 the antenna was decommissioned. Antenna coordinates are approximate; they were interpolated from coordinates for DSS-13 and DSS-14 in Table 5 of module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005) using the map at https://www.gdscc.nasa.gov/?page_id=37
• telescope : Leura Observatory 0.25-m
  The 0.25m is a 25 cm telescope located at -33.706833, 150.341694 at the Leura. Leura Observatory 0.25-m
• telescope : Lick Observatory 3.05-m Shane reflector
  The 3.05-m Shane reflector is a 3.05 m telescope located at 37.343109, 238.363922 at the Lick Observatory. Operational 1959+
• telescope : Lowell Observatory 21-in Reflector
  21.0-in (53 cm) reflector telescope at Lowell Observatory, Mars Hill, Flagstaff, AZ, was built for Harold Johnson, in 1953. The telescope ushered in photoelectric astronomy at Lowell. The 21-in is the only manually slewed telescope at Lowell and is still in use with minimal upgrades since 1953.
• telescope : Lowell Discovery Telescope (LDT)
  The Lowell Discovery Telescope, formerly known as the "Discovery Channel Telescope (DCT)", is a 4.3m diameter telescope with an effective focal length of 26.04 m and an f/ratio of 6.2. The LDT instrument cube allows simultaneous attachment of five instruments to the telescope.
• telescope : John S. Hall Telescope 1.07-m Hall Ritchey-Chretien Reflector
  The 1.07-meter Hall Ritchey-Chrétien reflector, also known as the John S. Hall Telescope, is located at Lowell Observatory's Anderson Mesa Station near Flagstaff, Arizona. Installed in 1970 and named in honor of former Lowell director John S. Hall in 1990, this telescope has been instrumental in various astronomical studies. In 2004, it underwent significant upgrades, including the installation of a new mirror from Hextek, enhancing its observational capabilities.
• telescope : Lowell Observatory Near-Earth-Object Search (LONEOS) 0.6m Schmidt Telescope
  The LONEOS 0.6-meter Schmidt Telescope, situated at Lowell Observatory's Anderson Mesa Station near Flagstaff, Arizona, was central to the Lowell Observatory Near-Earth-Object Search (LONEOS) from 1993 to 2008. Originally built in 1939 and acquired from Ohio Wesleyan University in 1990, the telescope underwent significant modifications, including the installation of a 16-megapixel CCD camera, enabling it to survey up to 1,000 square degrees of sky per night to a limiting visual magnitude of approximately 19.3 . Throughout its operation, LONEOS discovered over 22,000 minor planets, including more than 100 near-Earth asteroids, contributing significantly to planetary defense efforts.
• telescope : National Undergraduate Research Observatory (NURO) 0.79m (31inch) Telescope
  The information was adapted from Lowell Observatory web pages. This 0.79-meter (31-inch) telescope was installed in 1964 at Lowell’s Anderson Mesa Dark Sky Site. The U.S. Geological Survey originally operated it to create geological maps of the Moon, in support of Project Apollo. Ownership was transferred to Lowell Observatory in 1972, and it was refurbished in 1990. This telescope later became a primary research tool for the National Undergraduate Research Observatory (NURO). The effective focal length is 11.78 m, and the f/ratio is 15. The 31-inch telescope is stopped down to 29.5 inches (0.75m). The plate scale is 17 arcsec/mm.
• telescope : Perkins Warner and Swasey 1.83-m Telescope
  The 1.83-m Perkins Warner and Swasey reflector is a 1.83 m telescope located at 35.096832, 248.464081 at the Anderson Mesa Station. Operational 1961+; from Perkins Obs.
• telescope : DSS-53 34-m Radio Telescope
  Deep Space Station 53 (DSS-53) is scheduled to become operational in early 2021. The antenna is very similar in structure to earlier 34-m DSN antennas; however the transmission and reception equipment is located underground rather than in a cone at the focal point of the dish. The radio signal is guided from the subreflector through a hole in the surface of the dish to the receiving equipment via a system of reflecting mirrors inside a large tube. The reverse path allows transmission. This 'beam waveguide' (BWG) design reduces weight on the reflecting surface, insulates electronics from environmental factors including dish movement, and simplifies maintenance. DSS-53 can transmit up to 20 kW at 7.1 GHz. It can receive simultaneous right- and left-circular polarization at 8.4 GHz and 32.0 GHz. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). The Madrid Deep Space Communications Complex (MDSCC) has been managed since December 2012 by Ingeniería de Sistemas para la Defensa de España. MDSCC is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain.
• telescope : DSS-54 34-m Radio Telescope
  Deep Space Station 54 (DSS-54) became operational in 1997. The antenna is very similar in structure to earlier 34-m DSN antennas; however the transmission and reception equipment is located underground rather than in a cone at the focal point of the dish. The radio signal is guided from the subreflector through a hole in the surface of the dish to the receiving equipment via a system of reflecting mirrors inside a large tube. The reverse path allows transmission. This 'beam waveguide' (BWG) design reduces weight on the reflecting surface, insulates electronics from environmental factors including dish movement, and simplifies maintenance. DSS-54 can transmit up to 20 kW at 2.1 and 7.1 GHz. It can receive right- or left-circular polarization at 2.2, 8.4, and 26.2 GHz. At 32.0 GHz it can receive both polarizations simultaneously. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). The Madrid Deep Space Communications Complex (MDSCC) has been managed since December 2012 by Ingeniería de Sistemas para la Defensa de España. MDSCC is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain.
• telescope : DSS-55 34-m Radio Telescope
  Deep Space Station 55 (DSS-55) became operational in 2003. The antenna is very similar in structure to earlier 34-m DSN antennas; however the transmission and reception equipment is located underground rather than in a cone at the focal point of the dish. The radio signal is guided from the subreflector through a hole in the surface of the dish to the receiving equipment via a system of reflecting mirrors inside a large tube. The reverse path allows transmission. This 'beam waveguide' (BWG) design reduces weight on the reflecting surface, insulates electronics from environmental factors including dish movement, and simplifies maintenance. DSS-55 can transmit up to 20 kW at 7.1 GHz; it is expected to have an 800 W transmitter at 34.5 GHz by late 2024. It can receive simultaneous right- and left-circularly polarized signals at 8.4 and 32.0 GHz. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). The Madrid Deep Space Communications Complex (MDSCC) has been managed since December 2012 by Ingeniería de Sistemas para la Defensa de España. MDSCC is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain.
• telescope : DSS-56 34-m Radio Telescope
  Deep Space Station 56 (DSS-56) is scheduled to become operational in September 2020. The antenna is very similar in structure to earlier 34-m DSN antennas; however, the transmission and reception equipment is located underground rather than in a cone at the focal point of the dish. The radio signal is guided from the subreflector through a hole in the surface of the dish to the receiving equipment via a system of reflecting mirrors inside a large tube. The reverse path allows transmission. This 'beam waveguide' (BWG) design reduces weight on the reflecting surface, insulates electronics from environmental factors including dish movement, and simplifies maintenance. DSS-56 can transmit up to 250 W at 2.1 GHz and up to 20 kW at 7.1 GHz. It can receive right- or left-circular polarization at 2.2 GHz and 26.2 GHz; it can receive both polarizations simultaneously at 8.4 and 32.0 GHz. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). The Madrid Deep Space Communications Complex (MDSCC) has been managed since December 2012 by Ingeniería de Sistemas para la Defensa de España. MDSCC is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain.
• telescope : DSS-61 26-m Radio Telescope
  Deep Space Station 61 (DSS-61) is located at the Madrid Deep Space Communications Complex near Madrid, Spain. It became part of the NASA Deep Space Network in the mid 1960s. Its original diameter was 26-m, but that was extended to 34-m in the 1980s. The Madrid Deep Space Communications Complex (MDSCC) is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain. Under an agreement between the governments of Spain and the United States, dated 1964-01-29, the National Institute for Aerospace Technology (INTA) and the U.S. space agency NASA signed a contract for operation and maintenance of the MDSCC facilities.
• telescope : DSS-61 34-m Radio Telescope
  Deep Space Station 61 (DSS-61) is located at the Madrid Deep Space Communications Complex (MDSCC) near Madrid, Spain. It became part of the NASA Deep Space Network in the mid 1960s. Its original diameter was 26-m, but that was extended to 34-m in the 1980s. DSS-61 was decommissioned in 1999 and transferred to the PARTNeR Project (for educational purposes) in 2001. The Madrid Deep Space Communications Complex (MDSCC) is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain. Under an agreement between the governments of Spain and the United States, dated 1964-01-29, the National Institute for Aerospace Technology (INTA) and the U.S. space agency NASA signed a contract for operation and maintenance of the MDSCC facilities. The creation, in 1992, of the state-owned Aerospace Engineering and Services, SA (INSA, S.A.) under INTA, allowed the concentration of these responsibilities in the new company. INSA has disappeared and Ingeniería de Sistemas para la Defensa de España is the company that has managed MDSCC since December 2012.
• telescope : DSS-63 64-m Radio Telescope
  This fully steerable telescope is a parabolic reflector radio antenna that is part of the NASA Deep Space Network. It was first operational in 1974 with a 64-m aperture. The aperture was extended to 70-m in the late-1980s to support the Voyager 2 encounter with Neptune. The 64-m antenna could receive at frequencies between about 1.6 and 8.6 GHz in left-circular polarization (LCP); over 2.0-8.6 GHz it could receive simultaneously in right-circular poolarization (RCP). It could transmit up to 20 kW at 2.1 and 7.1 GHz. Antenna coordinates were converted from Table 5 in module 301 (revision L) of the DSN Telecommunications Link Design Handbook (DSN document 810-005). The Madrid Deep Space Communications Complex (MDSCC) is located about 65 km west of Madrid, near the town of Robledo de Chevala, Spain. Under an agreement between the governments of Spain and the United States, dated 1964-01-29, the National Institute for Aerospace Technology (INTA) and the U.S. space agency NASA signed a contract for operation and maintenance of the MDSCC facilities.

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