AMiBA
AMiBA during construction in 2006
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| Location(s) |
Mauna Loa  , United States of America
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| Coordinates | 19°32′10″N 155°34′31″W / 19.536194°N 155.575278°WCoordinates: 19°32′10″N 155°34′31″W / 19.536194°N 155.575278°W |
| Altitude | 3,396 m (11,142 ft) |
| Wavelength | 3 mm (100 GHz) |
| Built | 2000–2006 |
| First light | September 2006
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| Telescope style |
radio telescope, radio interferometer
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| Diameter | 0.576 m (1 ft 10.7 in) |
| Angular resolution | 6 minute of arc, 2 minute of arc
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| Mounting | Hexapod |
| Enclosure |
Retractable roof
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| Website | amiba |
 Location of AMiBA in United States of America.
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The Yuan-Tseh Lee Array for Microwave Background Anisotropy, also known as the Array for Microwave Background Anisotropy (AMiBA), is a radio telescope designed to observe the cosmic microwave background and the Sunyaev-Zel'dovich effect in clusters of galaxies. It is located on Mauna Loa in Hawaii, at 3,396 metres (11,142 ft) above sea level.
AMiBA was originally configured as a 7-element interferometer atop a hexapod mount. Observations at a wavelength of 3 mm (86–102 GHz) started in October 2006, and the detections of six clusters by the Sunyaev-Zel'dovich effect were announced in 2008. In 2009 the telescope was upgraded to 13 elements, and it is capable of further expansion to 19 elements. AMiBA is the result of a collaboration between the Academia Sinica Institute of Astronomy and Astrophysics, the National Taiwan University and the Australia Telescope National Facility, and also involves researchers from other universities.
AMiBA was initially configured as a 7-element interferometer, using 0.576 m Cassegrain dishes mounted on a 6 m carbon fibre hexapod mount. It is located on Mauna Loa, Hawaii, and observes at 3 mm (86–102 GHz) to minimize foreground emission from other, non-thermal sources. The telescope has a retractable shelter, made from seven steel trusses and PVC fabric.
The receivers are based on Monolithic Microwave Integrated Circuit (MMIC) technology, with low noise amplifiers cooled to 15 K, which have 20 GHz bandwidths and provide 46 dB of amplification. The signals are mixed with a local oscillator to reduce their frequency, prior to correlation with an analog correlator. The system temperatures are between 55 and 75 K.
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