The camera of the fifth H.E.S.S. telescope. Part I: System description

Bolmont, J.; Corona, P.; Gauron, P.; Ghislain, Patrick; Goffin, C.; Riveros, L. Guevara; Huppert, J.-F.; Martineau‐Huynh, O.; Nayman, P.; Parraud, Jean-Marc; Tavernet, J.‐P.; Toussenel, F.; Vincent, D.; Vincent, P.; Bertoli, W.; Espigat, P.; Punch, M.; Besin, D.; Delagnes, É.; Glicenstein, J. F.; Moudden, Y.; Venault, Philippe; Zaghia, H.; Brunetti, L.; p., David; Dubois, Jean; Fiaßon, A.; Geffroy, N.; Monteiro, Inocencio; Journet, Laure; Krayzel, F.; Lamanna, G.; Flour, T. Le; Lees, Sidney; Lieunard, B.; Maurin, G.; Mugnier, P.; Panazol, J. L.; Prast, J.; Chounet, L.‐M.; Degrange, B.; Edy, Evelyne; Fontaine, G.; Giebels, B.; Hormigos, S.; Khélifi, B.; Manigot, P.; Maritaz, P.; Naurois, M. de; Compin, M.; Feinstein, F.; Fernández, D.; Méhault, J.; Rivoire, S.; Royer, S.; Sanguillon, Michèle; Vasileiadis, G.

doi:10.1016/j.nima.2014.05.093

Cited by 35 publications

(22 citation statements)

References 17 publications

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“…consisted of four 12 m diameter telescopes (CT1-4). A fifth telescope (CT5) with a larger mirror diameter of 28 m and newly designed camera [12] augmented the array in 2012, reducing the energy threshold significantly to below 100 GeV. This array configuration constitutes H.E.S.S.…”

mentioning

confidence: 99%

H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

Abdalla¹,

Abramowski²,

Aharonian³

et al. 2016

Phys. Rev. Lett.

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confidence: 99%

H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

Abdalla¹,

Abramowski²,

Aharonian³

et al. 2016

Phys. Rev. Lett.

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“…with E 0 = 5 GeV for runs where the large H.E.S.S. telescope CT5 (see [14]) took part in the observation and E 0 = 30 GeV for all other runs. ε max corresponds to the maximum of the relative optical efficiencies of the observing IACTs, or directly to the one of CT5, if participating.…”

Section: Simulation Parameter Settingsmentioning

confidence: 99%

A run-wise simulation and analysis framework for Imaging Atmospheric Cherenkov Telescope arrays

Holler

Lenain

Naurois

et al. 2020

Astroparticle Physics

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We introduce a new simulation and analysis paradigm for Imaging Atmospheric Cherenkov Telescope (IACT) arrays, simulating the actual observation conditions as well as individual telescope configuration for each observation unit. Compared to existing frameworks, where simulations are usually generated using pre-defined settings, this run-wise simulation approach implies more realistic simulations and hence reduced systematic uncertainties. The computational effort of this dedicated simulation concept is notably independent of the amount of different observation configurations but just scales linearly with observation time. This corresponds to a large advantage for increasingly complex current and future IACT arrays where the size of the phase space makes it computationally unfeasible to generate simulations that reach the requirements regarding systematics using the classical simulation scheme.

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“…Each of the telescopes, located at the corners of a square with a side length of 120 m, has an effective mirror surface area of 107 m 2 , and is able to detect cosmic gamma-rays in the energy range 0.1-50 TeV. In 2012 October, a fifth telescope CT5, with an effective mirror surface area of 600 m 2 and an improved camera (Bolmont et al 2014), was installed at the centre of the original square, giving access to energies below 100 GeV (H.E.S.S. Collaboration et al 2017).…”

Section: H E S S O B S E Rvat I O N Smentioning

confidence: 99%

H.E.S.S. observations of the flaring gravitationally lensed galaxy PKS 1830–211

Abdalla

Aharonian

Benkhali

et al. 2019

Monthly Notices of the Royal Astronomical Society

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PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of ∼67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum.

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The camera of the fifth H.E.S.S. telescope. Part I: System description

Cited by 35 publications

References 17 publications

H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

A run-wise simulation and analysis framework for Imaging Atmospheric Cherenkov Telescope arrays

H.E.S.S. observations of the flaring gravitationally lensed galaxy PKS 1830–211

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