Auger@TA: An Auger-like surface detector micro-array embedded within the Telescope Array Project
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(Published version)
Date
2024
Authors
Mayotte, S.
Caraça-Valente, J.
Covault, C.
Fujii, T.
Im, S.
James, R.
Johnsen, J.
Kampert, K.H.
Kern, H.
Matthews, J.N.
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Conference paper
Citation
Proceedings of Science, 2024, vol.444, pp.368-1-368-15
Statement of Responsibility
S. Mayotte, J. Caraça-Valente, C. Covault, T. Fujii, S. Im, R. James, J. Johnsen, K.H. Kampert, H. Kern, J.N. Matthews, E. Mayotte, A. Bartz Mocellin, S. Quinn, H. Que, J. Rautenberg, M. Roth, H. Sagawa, T. Sako, F. Sarazin, R. Sato, D. Schmidt, S.B. Thomas, and G. Wörner, for the Pierre Auger and Telescope Array Collaborations
Conference Name
38th International Cosmic Ray Conference (ICRC) (26 Jul 2023 - 3 Aug 2023 : Nagoya, Japan)
Abstract
The Pierre Auger Observatory (Auger) and the Telescope Array Project (TA) are the two largest ultra-high-energy cosmic ray (UHECR) observatories in the world. One obstacle in pursuing full-sky UHECR physics is the apparent discrepancy in flux measured by the two experiments. This could be due to astrophysical differences as Auger and TA observe the Southern and Northern skies, respectively. However, the scintillation detectors used by TA have very different sensitivity to the various components of extensive air showers than the water-Cherenkov detectors (WCD) used by Auger. The discrepancy could also be due to systematic effects arising from the differing detector designs and reconstruction methods. The primary goal of the Auger@TA working group is to cross-calibrate the approaches of the two observatories using in-situ methods. This is achieved by placing a self-triggering micro-array, which consists of eight Auger surface detector stations, with both WCDs and AugerPrime scintillators, within the TA array. Seven of the WCDs use a 1-PMT prototype configuration and form a hexagon with the Auger spacing of 1.5 km. The eighth station uses a standard 3-PMT Auger WCD, placed with a TA station at the center of the hexagon to form a triplet for high-statistics, low-uncertainty, cross-calibration of instrumentation. Deployment of the micro-array took place between September 2022 and August 2023, with data-taking foreseen by the Fall of 2023. Details on the instrumentation and deployment of the micro-array, as well as its expected performance, trigger efficiencies, and event rate will be presented. First data from individual stations will also be shown.
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© Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0).