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Line 1: {{about\|the [[physics experiment]]\|\|Hegra (disambiguation)}} ~~[[Image:Hegra.jpg\|right\|thumb\|300px\|Overview of the HEGRA site in 1997]]~~ {{pp-move-indef\|small=yes}} ~~[[Image:Hegra_and_not_bob_tubbs_2001.jpg\|right\|thumb\|300px\|Two HEGRA reflectors, with the [[Nordic Optical Telescope\|NOT]] in the background.]]~~ {{Infobox telescope\|locmapin=Canary Islands}} '''HEGRA''', which stands for ''High-Energy-Gamma-Ray Astronomy'', was an atmospheric [[Cherenkov effect\|Cherenkov]] telescope for [[Gamma-ray astronomy]]. With its various types of detectors, HEGRA took data between 1987 and 2002, at which point it was dismantled in order to build its successor, [[MAGIC (telescope)\|MAGIC]], at the same site.▼ [[Image:Hegra.jpg\|right\|thumb\|300px\|Overview of the HEGRA site in 1997]][[Image:hegra scint and air.png\|thumb\|300px\|'''Schematic designs of the scintillation and AIROBICC counters''']] ▲'''HEGRA''', which stands for ''~~High~~'H'''igh-~~Energy~~'''E'''nergy-~~Gamma~~'''G'''amma-Ray ~~Astronomy~~'''A'''stronomy, was an atmospheric [[Cherenkov effect\|Cherenkov]] telescope for [[Gamma-ray astronomy]]. With its various types of detectors, HEGRA took data between 1987 and 2002, at which point it was dismantled in order to build its successor, [[MAGIC (telescope)\|MAGIC]], at the same site. It was located at [[Roque de los Muchachos Observatory]] on [[La Palma]] at a height of 2200 m above sea level.<ref name=":0">{{Cite web \|title=High Energy Gamma Ray Astronomy (HEGRA) \|url=https://www.mpi-hd.mpg.de/hfm/HEGRA/HEGRA.html \|access-date=2024-02-01 \|website=www.mpi-hd.mpg.de}}</ref> It was operated by an international collaboration of research institutes and universities, such as the [[Max Planck Institute for Physics]] in Munich, the [[Universidad Complutense de Madrid]], the German [[Max Planck Institute for Nuclear Physics]], the [[University of Wuppertal]], [[the IFKKI in Kiel]] or the [[University of Hamburg]]. It consisted of several detector types for observing secondary particles from [[Air shower (physics)\|particle cascades]] in the atmosphere. The particle ~~cascardes~~cascades detected by HEGRA were produced by cosmic ray particles in the energy range of 10<sup>12</sup>{{nbsp}}eV to 10<sup>16</sup>{{nbsp}}eV.<ref name=":0" /> The detectors with the lowest energy threshold were the ''atmospheric Cherenkov telescopes'' with "cameras" of photomultiplier tubes. They were sensitive to showers above 10<sup>12</sup>{{nbsp}}eV (1 TeV) but had to look towards possible sources and could be operated only during clear, moonless nights. They detected [[Cherenkov effect\|Cherenkov light]] from relativistic secondary particles in the air showers. The field of view was about 4.6~~°~~°. There were a total of six of these telescopes in operation. They were dismantled in September 2002. The reflectors of the telescope is 3.9 meter in diameter and consisted of 30 spherical mirrors.<ref>{{Cite journal \|last=Akhperjanian \|first=A. \|last2=Kankanian \|first2=R. \|last3=Sahakian \|first3=V. \|last4=Heusler \|first4=A. \|last5=Wiedner \|first5=C.-A. \|last6=Wirth \|first6=H. \|date=1998-06-01 \|title=The Optical Layout Of The HEGRA Cherenkov Telescopes \|url=https://doi.org/10.1023/A:1007915512981 \|journal=Experimental Astronomy \|language=en \|volume=8 \|issue=2 \|pages=135–152 \|doi=10.1023/A:1007915512981 \|issn=1572-9508}}</ref> The area of the reflector is 5 m<sup>2</sup>.<ref>{{Cite journal \|last=Mirzoyan \|first=R. \|last2=Kankanian \|first2=R. \|last3=Krennrich \|first3=F. \|last4=Müller \|first4=N. \|last5=Sander \|first5=H. \|last6=Sawallisch \|first6=P. \|last7=Aharonian \|first7=F. \|last8=Akhperjanian \|first8=A. \|last9=Beglarian \|first9=A. \|last10=Fernandez \|first10=J. \|last11=Fonseca \|first11=V. \|last12=Grewe \|first12=W. \|last13=Heusler \|first13=A. \|last14=Konopelko \|first14=A. K. \|last15=Lorenz \|first15=E. \|date=1994-12-01 \|title=The first telescope of the HEGRA air Cherenkov imaging telescope array \|url=https://www.sciencedirect.com/science/article/pii/0168900294913811 \|journal=Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment \|volume=351 \|issue=2 \|pages=513–526 \|doi=10.1016/0168-9002(94)91381-1 \|issn=0168-9002}}</ref> ~~[[Image:hegra_scint_and_air.png\|thumb\|left\|300px\|Shematic designs of the scintilation and AIROBICC counters]]~~ Another detector type for Cherenkov light was '''AIROBICC''' ('''AIR'''shower '''O'''bservation '''B'''y angle '''I'''ntegrating '''C'''herenkov '''C'''ounters) with one large photomultiplier looking at the sky above it. 49 of these detectors were spread in a 7-by-7 grid to observe the amplitude and the time of arrival of the front of Cherenkov light. Another 48 were added later on. These counters had a wide field of view but ~~couldn~~could only be operated during clear, moonless nights, like the atmospheric Cherenkov telescopes. Their energy threshold was a few 10<sup>13</sup>{{nbsp}}eV. The AIROBICC array has been dismantled. The first detector type of HEGRA was the array of 1 m<sup>2</sup> scintillation counters which were used to measure the numbers and arrival times of secondary particles in air showers arriving at ground level. More than 250 of these Line 15 ⟶ 18: The scintillator array was sensitive to all types of charged secondary particles. To be able to select secondary muons in air showers there were the Muon 'Towers' with 16 m<sup>2</sup> area each. Seventeen of these detectors were installed on La Palma. There were two more types of detectors at the HEGRA site: the CRT (Cosmic Ray Tracking)[http://www.mpi-hd.mpg.de/hfm/CRT/CRT.html] and the CLUE (Cherenkov Light Ultraviolet Experiment)[http://www.pi.infn.it/clue/] {{Webarchive\|url=https://web.archive.org/web/20200520053233/https://www.pi.infn.it/clue/ \|date=2020-05-20 }}. [[Image:Shower detection.png\|thumb\|right\|400px\|Schematic representation of cosmic ray shower detection]] A remarkable achievement of the instrument was the detection of the most energetic photons observed from an extragalactic object, at 16 [[TeV]], originating from [[Markarian 501]] (Mrk 501). It was shut down in [[2002]] in order to build the ~~followup~~follow-up telescope [[MAGIC (telescope)\|MAGIC]] at the same site. A direct successor to the stereoscopic system of Cherenkov telescopes is the [[HESS]] experiment. ~~<BR CLEAR="ALL">~~ ==See Also==▼ ▲==See ~~Also~~also== * The [[MAGIC (telescope)\|MAGIC Telescope]], successor to HEGRA ==References== {{reflist}} ==External links== * [https://web.archive.org/web/20050209034041/http://www-hegra.desy.de/hegra/ The official HEGRA site] * [http://www.mpi-hd.mpg.de/hfm/CT/CT.html The HEGRA Atmospheric Cherenkov Telescope System ] * [http://www.mpi-hd.mpg.de/hfm/CosmicRay/Showers.html Cosmic ray showers] * [http://www.mpi-hd.mpg.de/HESS HESS] {{DEFAULTSORT:Hegra}} [[Category:Gamma-ray telescopes]] [[Category:Astronomical observatories in La Palma]] [[Category:Cosmic-ray telescopes]]