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Green Bank Telescope
The Robert C. Byrd Green Bank Telescope (GBT) in Green Bank, West Virginia, US is the world's largest fully steerable radio telescope, surpassing the Effelsberg 100-m Radio Telescope in Germany. The Green Bank site was part of the National Radio Astronomy Observatory (NRAO) until September 30, 2016. Since October 1, 2016, the telescope has been operated by the independent Green Bank Observatory. The telescope's name honors the late Senator Robert C. Byrd who represented West Virginia and who pushed the funding of the telescope through Congress.
The Green Bank Telescope operates at meter to millimeter wavelengths. Its 100-meter-diameter collecting area, unblocked aperture, and good surface accuracy provide superb sensitivity across the telescope's full 0.1–116 GHz operating range. The GBT is fully steerable, and 85 percent of the local celestial hemisphere is accessible. It is used for astronomy about 6500 hours out of the 8760 hours in a year, with 2000–3000 hours per year going to high-frequency science. Part of the scientific strength of the GBT is its flexibility and ease of use, allowing for rapid response to new scientific ideas and phenomena. It is scheduled dynamically to match project needs to the available weather. The GBT is also readily reconfigured with new and experimental hardware. The high-sensitivity mapping capability of the GBT makes it a vital complement to the Atacama Large Millimeter Array, the Expanded Very Large Array, the Very Long Baseline Array, and other high-angular-resolution interferometers. Facilities of the Green Bank Observatory are also used for other scientific research, for many programs in education and public outreach, and for training students and teachers.
The telescope began regular science operations in 2001, making it one of the newest astronomical facilities of the US National Science Foundation (NSF). It was constructed following the collapse of a previous telescope at Green Bank, the 300 Foot Radio Telescope, a 90.44 m paraboloid that began observations in October 1961. This previous telescope collapsed on 15 November 1988 due to the failure of a gusset plate in the box girder assembly, which was a key component for the structural integrity of the telescope.
The telescope sits near the heart of the United States National Radio Quiet Zone, a unique area located in the town of Green Bank, West Virginia, where authorities limit all radio transmissions to avoid emissions toward the GBT and the Sugar Grove Station. The location of the telescope within the Radio Quiet Zone allows for the detection of faint radio-frequency signals which human-made signals might otherwise mask. The observatory borders National Forest land, and the Allegheny Mountains shield it from some radio interference.
The telescope's location has been the site of important radio astronomy telescopes since 1957. It currently houses seven additional telescopes, and in spite of its somewhat remote location, receives about 40,000 visitors each year.
The structure weighs 7,600 metric tons (8,400 short tons) and is 485 feet (148 m) tall. The surface area of the GBT is a 100-by-110-meter active surface with 2,209 actuators (small motors used to adjust the position) for the 2,004 surface panels, making the total collecting area of 2.3 acres (9,300 m2). The panels are made from aluminum manufactured to a surface accuracy of better than 50 micrometres (0.0020 in) RMS. The actuators adjust the panel positions to compensate for sagging, or bending under its own weight, which changes as the telescope moves. Without this so-called "active surface" adjustment, observations at frequencies above 4 GHz would not be as efficient.
Unusual for a radio telescope, the primary reflector is an off-axis segment of a paraboloid. This is the same design used in smaller (eg., 45–100 cm) home satellite television dishes. The asymmetric reflector allows the telescope's focal point and feed horn to be located at the side of the dish, so that it and its retractable support boom do not obstruct the incoming radio waves, as occurs in conventional radio telescope designs with the feed located on the telescope's beam axis.
The 200-foot (61 m) offset support arm houses a prime focus receiver on a retractable boom in front of a subreflector, and a receiver room. For prime focus operation, the boom is extended to position the feed horn in front of the 8 m subreflector. For Gregorian focus operation, the prime focus boom is retracted. The subreflector, positioned by a Stewart platform with 6 degrees of freedom, reflects incoming radio waves toward eight higher-frequency feeds on a rotating turret located on top of the receiver room. The computerized controlled turret can rotate a particular receiver into the position within a few minutes. Operational frequencies range from 290 MHz to 115 GHz.
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Green Bank Telescope
The Robert C. Byrd Green Bank Telescope (GBT) in Green Bank, West Virginia, US is the world's largest fully steerable radio telescope, surpassing the Effelsberg 100-m Radio Telescope in Germany. The Green Bank site was part of the National Radio Astronomy Observatory (NRAO) until September 30, 2016. Since October 1, 2016, the telescope has been operated by the independent Green Bank Observatory. The telescope's name honors the late Senator Robert C. Byrd who represented West Virginia and who pushed the funding of the telescope through Congress.
The Green Bank Telescope operates at meter to millimeter wavelengths. Its 100-meter-diameter collecting area, unblocked aperture, and good surface accuracy provide superb sensitivity across the telescope's full 0.1–116 GHz operating range. The GBT is fully steerable, and 85 percent of the local celestial hemisphere is accessible. It is used for astronomy about 6500 hours out of the 8760 hours in a year, with 2000–3000 hours per year going to high-frequency science. Part of the scientific strength of the GBT is its flexibility and ease of use, allowing for rapid response to new scientific ideas and phenomena. It is scheduled dynamically to match project needs to the available weather. The GBT is also readily reconfigured with new and experimental hardware. The high-sensitivity mapping capability of the GBT makes it a vital complement to the Atacama Large Millimeter Array, the Expanded Very Large Array, the Very Long Baseline Array, and other high-angular-resolution interferometers. Facilities of the Green Bank Observatory are also used for other scientific research, for many programs in education and public outreach, and for training students and teachers.
The telescope began regular science operations in 2001, making it one of the newest astronomical facilities of the US National Science Foundation (NSF). It was constructed following the collapse of a previous telescope at Green Bank, the 300 Foot Radio Telescope, a 90.44 m paraboloid that began observations in October 1961. This previous telescope collapsed on 15 November 1988 due to the failure of a gusset plate in the box girder assembly, which was a key component for the structural integrity of the telescope.
The telescope sits near the heart of the United States National Radio Quiet Zone, a unique area located in the town of Green Bank, West Virginia, where authorities limit all radio transmissions to avoid emissions toward the GBT and the Sugar Grove Station. The location of the telescope within the Radio Quiet Zone allows for the detection of faint radio-frequency signals which human-made signals might otherwise mask. The observatory borders National Forest land, and the Allegheny Mountains shield it from some radio interference.
The telescope's location has been the site of important radio astronomy telescopes since 1957. It currently houses seven additional telescopes, and in spite of its somewhat remote location, receives about 40,000 visitors each year.
The structure weighs 7,600 metric tons (8,400 short tons) and is 485 feet (148 m) tall. The surface area of the GBT is a 100-by-110-meter active surface with 2,209 actuators (small motors used to adjust the position) for the 2,004 surface panels, making the total collecting area of 2.3 acres (9,300 m2). The panels are made from aluminum manufactured to a surface accuracy of better than 50 micrometres (0.0020 in) RMS. The actuators adjust the panel positions to compensate for sagging, or bending under its own weight, which changes as the telescope moves. Without this so-called "active surface" adjustment, observations at frequencies above 4 GHz would not be as efficient.
Unusual for a radio telescope, the primary reflector is an off-axis segment of a paraboloid. This is the same design used in smaller (eg., 45–100 cm) home satellite television dishes. The asymmetric reflector allows the telescope's focal point and feed horn to be located at the side of the dish, so that it and its retractable support boom do not obstruct the incoming radio waves, as occurs in conventional radio telescope designs with the feed located on the telescope's beam axis.
The 200-foot (61 m) offset support arm houses a prime focus receiver on a retractable boom in front of a subreflector, and a receiver room. For prime focus operation, the boom is extended to position the feed horn in front of the 8 m subreflector. For Gregorian focus operation, the prime focus boom is retracted. The subreflector, positioned by a Stewart platform with 6 degrees of freedom, reflects incoming radio waves toward eight higher-frequency feeds on a rotating turret located on top of the receiver room. The computerized controlled turret can rotate a particular receiver into the position within a few minutes. Operational frequencies range from 290 MHz to 115 GHz.
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