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==Surface detector==
[[File:SurfaceDetection.svg|thumb|A Scintillator Surface Detector from Telescope Array]]
The surface detectors that make up the ground array are activated when ionizing particles from an extensive air shower pass through them. When these particles pass through the plastic scintillator within the detector, it induces photo electrons which are then gathered by wavelength-shifting fibers and sent to a photomultiplier tube. The electronic components within the detectors then filter the results, giving the detectors comparable accuracy to the AGASA experiment.<ref name=Kawai2008>{{cite journal|last=Kawai|first=H|display-authors=etal |title=Telescope Array Experiment|journal=Nuclear Physics B: Proceedings Supplements|volume=175-176|date=2008|pages=220–226|doi=10.1016/j.nuclphysbps.2007.11.002|bibcode = 2008NuPhS.175..221K }}</ref>
The surface detectors are evenly distributed across a 762 km<sup>2</sup> grid array with 1.2 km between each unit. Each surface detector has an assembled weight of 250 kg and consists of a power supply, two layers of scintillation detectors and electronics. Power is generated by a 120W solar panel and stored in a sealed lead-acid battery. The system has the capacity to operate for one week in complete darkness. Each scintillation detector layer is made of extruded plastic scintillator that is 1.2 cm thick and has an area of 3m<sup>2</sup>. The photo multiplier tube is connected to the scintillator via 96 wavelength-shifting fibers.
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The Telescope Array has three fluorescence detector (FD) telescope stations. As in the previous Fly's Eye and [[High Resolution Fly's Eye Cosmic Ray Detector|High Resolution Fly's Eye]] (HiRes) experiments, these detectors work by measuring the air fluorescence light emitted by an [[Air shower (physics)|extensive air shower]]. Each FD telescope consists of a primary mirror (made up of 18 smaller hexagonal mirror segments) and a camera. The cameras are made up of 256 PMTs (photomultiplier tubes) which are sensitive to the ultra violet light generated by a cosmic ray air shower.<ref name=Tokuno />
The stations are located on a triangle about 35 km apart from one another. Each station has 12-14 telescopes viewing the range from 3 to 33 degrees in elevation. The three sites are named ''Black Rock Mesa'' (BRM), ''Long Ridge'' (LR), and ''Middle Drum'' (MD).<ref>{{Cite web | url=http://www.telescopearray.org/index.php/research/clear-sky-clocks | title=Clear Sky Clocks}}</ref> By combining the data from the three sites, it is possible to determine the primary energy, the arrival direction, and the maximum
point of longitudinal development for an air shower.<ref name=Tokuno />
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