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Technical Physics
Erschienen in: Technical Physics 6/2020

01.06.2020 | PLASMA

The Application Potential of Silicon Photomultipliers for a Camera of a Small-Size Cherenkov Gamma-Ray Telescope for Reducing the Detection Threshold

verfasst von: E. E. Kholupenko, A. M. Krassilchtchikov, D. V. Badmaev, A. A. Bogdanov, Yu. V. Tuboltsev, Yu. V. Chichagov, A. S. Antonov, D. O. Kuleshov, E. M. Khil’kevich

Erschienen in: Technical Physics | Ausgabe 6/2020

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Abstract

Source and noise signals in a new camera of the TAIGA-IACT Cherenkov γ-ray telescope based on silicon photomultipliers (SiPM) have been simulated. It is shown that application of modern silicon photomultipliers as detecting elements of TAIGA-IACT (instead of the currently used conventional vacuum photomultipliers) will make it possible to reduce the threshold detection energy of cosmic γ quanta by a factor of about 2.5 (from ≃1.5 to ≃0.6 TeV). It is also shown that employment of a standard ZWB3 UV filter mask in the TAIGA-IACT camera would reduce the average signal level by a factor of about 3 and the noise (background) level from the night sky by a factor of about 6, which would allow one to extend the duty cycle of the telescope (in particular, to carry out observations during moonlit nights and twilights) and to additionally reduce the threshold detection energy down to ≃0.3 TeV. The application of a narrower UV filter of 260–300 nm bandwidth can increase the efficiency of determining the primary particle type (γ-hadron separation) in the energy range from ~25 up to ~50 TeV.
Vorheriger Artikel Investigation of Laser-Produced Plasma in a Dilute-Gas Environment by Means of a Single Electrostatic Probe
Nächster Artikel Ceramic Solid Solutions of Li0.17Na0.83TayNb1 –yO3: Thermobaric Synthesis, Microstructure, and Properties

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Fußnoten
1
Hereinafter, the term “EAS electrons” denotes secondary electrons and positrons of an EAS.
 
2
Note that, despite the use of the term “intensity” and designations Iλ and I, these parameters characterize particle fluxes (as it was assumed in [28]) rather than total energies of emitted photons and, in this sense, differ from the designations of [27].
 
3
This parameter should not be confused with the pixel field of view, which equals to 35° [15] and allows each pixel to “observe” all portions of the telescope mirror.
 
4
In the case of vertical incidence, the distance to the EAS axis coincides with the primary-particle impact parameter.
 
5
The standard deviations of Vm(λ), VW(λ), PDE(λ), and F(λ) are neglected in (8).
 
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Metadaten
Titel
The Application Potential of Silicon Photomultipliers for a Camera of a Small-Size Cherenkov Gamma-Ray Telescope for Reducing the Detection Threshold
verfasst von
E. E. Kholupenko
A. M. Krassilchtchikov
D. V. Badmaev
A. A. Bogdanov
Yu. V. Tuboltsev
Yu. V. Chichagov
A. S. Antonov
D. O. Kuleshov
E. M. Khil’kevich
Publikationsdatum
01.06.2020
Verlag
Pleiades Publishing
Erschienen in
Technical Physics / Ausgabe 6/2020
Print ISSN: 1063-7842
Elektronische ISSN: 1090-6525
DOI
https://doi.org/10.1134/S1063784220060158

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