Evaluation of the effective mirror area of CTA Small-Sized Telescopes for camera design and Monte Carlo simulation
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A90247%2F24%3A00643271" target="_blank" >RIV/68378271:90247/24:00643271 - isvavai.cz</a>
Výsledek na webu
<a href="https://pos.sissa.it/444/675/pdf" target="_blank" >https://pos.sissa.it/444/675/pdf</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.22323/1.444.0675" target="_blank" >10.22323/1.444.0675</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
Evaluation of the effective mirror area of CTA Small-Sized Telescopes for camera design and Monte Carlo simulation
Popis výsledku v původním jazyce
The effective mirror area of an imaging atmospheric Cherenkov telescope is a crucial key parameter for trigger threshold determination and energy calibration. It is usually calculated by 3D ray-tracing simulation using a simplified telescope model, and the result is used in Monte Carlo simulations. However, simplified telescope and camera models are not adequate for the Schwarzschild–Couder configuration to be used in Small-Sized Telescopes (SSTs) of the Cherenkov Telescope Array. This is because the complex 3D structure of the secondary mirror, telescope masts, and camera body block a significant fraction of Cherenkov and night-sky photons. To evaluate the effective mirror area of an SST and to finalize its camera body design with minimal shadowing, a complex 3D model was built and simulated using the ROBAST ray-tracing library. A camera body size of 570 mm and a window size of 430 mm were selected for the final camera design based on the evaluation of shadowing by simulation. A non-axisymmetric effective area distribution was determined via the modeling of the complex telescope structure, while meeting the SST effective area requirement.
Název v anglickém jazyce
Evaluation of the effective mirror area of CTA Small-Sized Telescopes for camera design and Monte Carlo simulation
Popis výsledku anglicky
The effective mirror area of an imaging atmospheric Cherenkov telescope is a crucial key parameter for trigger threshold determination and energy calibration. It is usually calculated by 3D ray-tracing simulation using a simplified telescope model, and the result is used in Monte Carlo simulations. However, simplified telescope and camera models are not adequate for the Schwarzschild–Couder configuration to be used in Small-Sized Telescopes (SSTs) of the Cherenkov Telescope Array. This is because the complex 3D structure of the secondary mirror, telescope masts, and camera body block a significant fraction of Cherenkov and night-sky photons. To evaluate the effective mirror area of an SST and to finalize its camera body design with minimal shadowing, a complex 3D model was built and simulated using the ROBAST ray-tracing library. A camera body size of 570 mm and a window size of 430 mm were selected for the final camera design based on the evaluation of shadowing by simulation. A non-axisymmetric effective area distribution was determined via the modeling of the complex telescope structure, while meeting the SST effective area requirement.
Klasifikace
Druh
D - Stať ve sborníku
CEP obor
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OECD FORD obor
10303 - Particles and field physics
Návaznosti výsledku
Projekt
—
Návaznosti
—
Ostatní
Rok uplatnění
2024
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název statě ve sborníku
Proceedings of Science
ISBN
—
ISSN
1824-8039
e-ISSN
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Počet stran výsledku
8
Strana od-do
675
Název nakladatele
Sissa Medilab srl
Místo vydání
Trieste
Místo konání akce
Nagoya
Datum konání akce
26. 7. 2023
Typ akce podle státní příslušnosti
WRD - Celosvětová akce
Kód UT WoS článku
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