PoS - Proceedings of Science
Volume 358 - 36th International Cosmic Ray Conference (ICRC2019) - GRI - Gamma Ray Indirect
The calibration of the first Large-Sized Telescope of the Cherenkov Telescope Array
S. Sakurai*, D. Depaoli, R. Lopez-Coto, J. Becerra González, A. Berti, O. Blanch, F. Casso, A. Chiavassa, D. Corti, A. De Angelis, C. Delgado, C. Díaz, F. Di Pierro, L. Di Venere, M. Doro, A. Fernández-Barral, F. Giordano, S. Griffiths, D. Hadasch, Y. Inome, L. Jouvin, D. Kerszberg, H. Kubo, A. López-Oramas, M. Mallamaci, M. Mariotti, G. Martinez, S. Masuda, D. Mazin, A. Moralejo, E. Moretti, T. Nagayoshi, D. Ninci, L. Nogués, S. Nozaki, A. Okumural, R. Paoletti, P. Penil, R. Pillera, C. Pio, R. Rando, F. Rotondo, A. Rugliancich, T. Saito, Y. Sunada, M. Suzuki, M. Takahashi, L. A. Tejedor, P. Vallania, C. Vigorito, T. Yamamoto, T. Yoshida  on behalf of the CTA Consortiumet al. (click to show)
Full text: pdf
Pre-published on: July 22, 2019
Published on: July 02, 2021
The Cherenkov Telescope Array (CTA) represents the next generation of very high-energy gamma-ray observatory, which will provide broad coverage of gamma rays from 20 GeV to 300 TeV with unprecedented sensitivity. CTA will employ three different sizes of telescopes, and the Large-Sized Telescopes (LSTs) of 23-m diameter dish will provide the sensitivity in the lowest energies down to 20 GeV. The first LST prototype has been inaugurated in October 2018 at La Palma (Canary Islands, Spain) and has entered the commissioning phase. The camera of the LST consists of 265 PMT modules. Each module is equipped with seven high-quantum-efficiency Photomultiplier Tubes (PMTs), a slow control board, and a readout board. Ensuring high uniformity and precise characterization of the camera is the key aspects leading to the best performance and low systematic uncertainty of the LST cameras. Therefore, prior to the installation on site, we performed a quality check of all PMT modules. Moreover, the absolute calibration of light throughput is essential to reconstruct the amount of light received by the telescope. The amount of light is affected by the atmosphere, by the telescope optical system and camera, and can be calibrated using the ring-shaped images produced by cosmic-ray muons. In this contribution, we will show the results of off-site quality control of PMT modules and on-site calibration using muon rings. We will also highlight the status of the development of Silicon Photomultiplier modules that could be considered as a replacement of PMT modules for further improvement of the camera.
DOI: https://doi.org/10.22323/1.358.0780
How to cite

Metadata are provided both in "article" format (very similar to INSPIRE) as this helps creating very compact bibliographies which can be beneficial to authors and readers, and in "proceeding" format which is more detailed and complete.

Open Access
Creative Commons LicenseCopyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.