PoS - Proceedings of Science
Volume 358 - 36th International Cosmic Ray Conference (ICRC2019) - CRI - Cosmic Ray Indirect
The AMIGA underground muon detector of the Pierre Auger Observatory - performance and event reconstruction
A.M. Botti*  on behalf of the Pierre Auger Collaboration
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Pre-published on: August 20, 2019
Published on: July 02, 2021
The Auger Muons and Infill for the Ground Array (AMIGA) aims to both lower the detection threshold of the Pierre Auger Observatory down to energies of $\sim 10^{16.5}$ eV and to directly measure the muon content of extensive air showers. AMIGA consists of an array of coupled water-Cherenkov and buried scintillation detectors deployed in two superimposed triangular grids of 433 m and 750 m spacings. Each underground detector has a total area of 30 $\mathrm{m}^2$ buried at a depth of 2.3 m, to shield it from the shower electromagnetic component. The scintillation plane is segmented in plastic-scintillator strips with embedded wavelength-shifter optical fibers coupled to a common optical sensor. Before proceeding to the construction of the full-size array, an engineering array was operated until November 2017 to validate and optimize the design, and to evaluate the performance of the detection system. During this phase, scintillation areas of 5 $\mathrm{m}^2$ and 10 $\mathrm{m}^2$ and two optical sensors, photomultiplier tubes and silicon photomultipliers, were tested. In this work, we present the status and performance of the array currently equipped with silicon photomultipliers, along with the timing performance and geometry reconstruction of modules equipped with photomultiplier tubes. Analyses and results are based on both laboratory and field measurements. Scintillation areas of 10 $\mathrm{m}^2$ and silicon photomultipliers as readout have been selected as the baseline design for the full-scale AMIGA array.
DOI: https://doi.org/10.22323/1.358.0202
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