The scintillator surface detector of the Pierre Auger observatory

Authors

A. Abdul Halim, The University of Adelaide
P. Abreu, Instituto Superior Técnico
M. Aglietta, Istituto Nazionale di Fisica Nucleare, Sezione di Torino
I. Allekotte, Centro Atomico Bariloche
K. Almeida Cheminant, Radboud Universiteit
A. Almela, Comision Nacional de Energia Atomica Argentina
R. Aloisio, Gran Sasso Science Institute
J. Alvarez-Muñiz, Instituto Galego de Física de Altas Enerxías (IGFAE)
A. Ambrosone, Gran Sasso Science Institute
J. Ammerman Yebra, Instituto Galego de Física de Altas Enerxías (IGFAE)
G. A. Anastasi, Istituto Nazionale di Fisica Nucleare, Sezione di Catania
L. Anchordoqui, Lehman College
B. Andrada, Comision Nacional de Energia Atomica Argentina
L. Andrade Dourado, Gran Sasso Science Institute
S. Andringa, Instituto Superior Técnico
L. Apollonio, Istituto Nazionale di Fisica Nucleare, Sezione di Milano
C. Aramo, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli
E. Arnone, Istituto Nazionale di Fisica Nucleare, Sezione di Torino
J. C. Arteaga Velázquez, Universidad Michoacana de San Nicolás de Hidalgo
R. Assiro, Istituto Nazionale di Fisica Nucleare, Sezione di Lecce
P. Assis, Instituto Superior Técnico
G. Avila, Comision Nacional de Energia Atomica Argentina
E. Avocone, Laboratori Nazionali del Gran Sasso
A. Bakalova, Institute of Physics of the Czech Academy of Sciences
F. Barbato, Gran Sasso Science Institute
A. Bartz Mocellin, Colorado School of Mines
K. H. Becker, Bergische Universität Wuppertal
J. A. Bellido, The University of Adelaide
C. Berat, Université Grenoble Alpes
M. E. Bertaina, Istituto Nazionale di Fisica Nucleare, Sezione di Torino
M. Bianciotto, Istituto Nazionale di Fisica Nucleare, Sezione di Torino

Document Type

Article

Publication Date

8-1-2025

Abstract

Data collected so far by the Pierre Auger Observatory have enabled major advances in ultrahigh energy cosmic ray physics and demonstrated that improved determination of masses of primary cosmic-ray particles, preferably on an event-by-event basis, is necessary for understanding their origin and nature. Improvement in primary mass measurements was the main motivation for the upgrade of the Pierre Auger Observatory, called AugerPrime. As part of this upgrade, scintillator detectors are added to the existing water-Cherenkov surface detector stations. By making use of the differences in detector response to the electromagnetic particles and muons between scintillator and water-Cherenkov detectors, the electromagnetic and muonic components of cosmic-ray air showers can be disentangled. Since the muonic component is sensitive to the primary mass, such combination of detectors provides a powerful way to improve primary mass composition measurements over the original Auger surface detector design. In this paper, the so-called Scintillator Surface Detectors are discussed, including their design characteristics, production process, testing procedure and deployment in the field.

Publication Title

Journal of Instrumentation

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