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A Weber bar is a device designed to detect gravitational waves, first devised and constructed by physicist Joseph Weber at the University of Maryland. The device consisted of aluminium cylinders, 2 meters in length and 1 meter in diameter , antennae for detecting gravitational waves .
The earliest type was the room-temperature bar-shaped antenna called a Weber bar; these were dominant in 1960s and 1970s and many were built around the world. It was claimed by Weber and some others in the late 1960s and early 1970s that these devices detected gravitational waves; however, other experimenters failed to detect gravitational ...
Allegro was a ground-based, cryogenic resonant Weber bar, gravitational-wave detector [1] run by Warren Johnson, et al. at Louisiana State University in Baton Rouge, Louisiana. The detector was commissioned in the early 1990s, and was decommissioned in 2008.
Weber had continued developing his bar detectors through the early 1960s iterating on their design and implementation to also reduce the amount of seismic and thermal noise the detector was exposed to, and by 1967 he believed his detectors were picking up signals indicative of gravitational waves. [16]
The CLIO detector, with 100 m arms and located in the Kamioka mine, is another test detector, specifically designed to test the cryogenic technology used in KAGRA. [ 18 ] LIGO-Australia is a defunct project which was envisioned to be built on the model of the LIGO detector in Australia, but was finally not funded by the Australian government ...
Joseph Weber (May 17, 1919 – September 30, 2000) was an American physicist. He gave the earliest public lecture on the principles behind the laser and the maser and developed the first gravitational wave detectors, known as Weber bars.
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Time–frequency representations (Chatterji et al. 2004) of data containing GW190814, observed by LIGO Hanford (top), LIGO Livingston (middle), and Virgo (bottom). Times are shown relative to 2019 August 14, 21:10:39 UTC. Each detector's data are whitened by their respective noise amplitude spectral density and a Q-transform is calculated.