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==Overview==
[[File:TelescopeArray.svg|thumb|left|An illustration of Telescope Array. Three fluorescence telescopes observe the ultraviolet light given off by an air shower, while an array of surface detectors register the particles as they strike the ground.]]
The Telescope Array observatory is a hybrid detector system consisting of both an array of 507 scintillation surface detectors (SD) which measure the distribution of charged particles at the Earth's surface, and three fluorescence stations which observe the night sky above the SD array.<ref name="AbuZayyad2012">T. AbuZayyad et al., "[http://www.telescopearray.org/media/TA_papers/1-s2.0-S0168900212005931-main.pdf The surface detector array of the Telescope Array experiment]" Nuclear Instruments and Methods in Physics Research Section A: (2012) vol. 689</ref> Each fluorescence station is also accompanied by a LIDAR system for atmospheric monitoring.<ref name="chikawaICRC">M. Chikawa et al., Proceedings of 29th [[International Cosmic Ray Conference|ICRC]] (2005) 137</ref> The SD array is much like that of the [[AGASA]] group, but covers an area that is nine times larger. The hybrid setup of the Telescope Array project allows for simultaneous observation of both the longitudinal development and the lateral distribution of the air showers. When a cosmic ray passes through the earth's atmosphere and triggers an [[Air shower (physics)|air shower]], the fluorescence telescopes measure the scintillation light generated as the shower passes through the gas of the atmosphere, while the array of scintillator surface detectors samples the footprint of the shower when it reaches the Earth's surface.
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==Surface detector==
[[File:SurfaceDetection.svg|
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|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.
==FD station, telescope, and camera==
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point of longitudinal development for an air shower.<ref name=Tokuno />
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