Trigger and aperture of the surface detector array of the Pierre Auger Observatory

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The surface detector array of the Pierre Auger Observatory consists of 1600 water-Cherenkov detectors, for the study of extensive air showers (EAS) generated by ultra-high-energy cosmic rays. We describe the trigger hierarchy, from the identification of candidate showers at the level of a single det...

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Autor principal:	Multitudinario:475
Formato:	JOUR
Materias:	Auger Observatory Exposure Extensive air showers Trigger Ultra high energy cosmic rays Augers Cosmology Observatories Particle detectors Auger observatory Ultra high-energy cosmic rays Cosmic rays
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_01689002_v613_n1_p29_Multitudinario
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_01689002_v613_n1_p29_Multitudinario
record_format	dspace
spelling	todo:paper_01689002_v613_n1_p29_Multitudinario2023-10-03T15:06:44Z Trigger and aperture of the surface detector array of the Pierre Auger Observatory Multitudinario:475 Auger Observatory Exposure Extensive air showers Trigger Ultra high energy cosmic rays Augers Cosmology Observatories Particle detectors Auger observatory Exposure Extensive air showers Trigger Ultra high-energy cosmic rays Cosmic rays The surface detector array of the Pierre Auger Observatory consists of 1600 water-Cherenkov detectors, for the study of extensive air showers (EAS) generated by ultra-high-energy cosmic rays. We describe the trigger hierarchy, from the identification of candidate showers at the level of a single detector, amongst a large background (mainly random single cosmic ray muons), up to the selection of real events and the rejection of random coincidences. Such trigger makes the surface detector array fully efficient for the detection of EAS with energy above 3 × 10 18 eV, for all zenith angles between 0 {ring operator} and 60 {ring operator} , independently of the position of the impact point and of the mass of the primary particle. In these range of energies and angles, the exposure of the surface array can be determined purely on the basis of the geometrical acceptance. © 2009 Elsevier B.V. All rights reserved. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_01689002_v613_n1_p29_Multitudinario
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Auger Observatory Exposure Extensive air showers Trigger Ultra high energy cosmic rays Augers Cosmology Observatories Particle detectors Auger observatory Exposure Extensive air showers Trigger Ultra high-energy cosmic rays Cosmic rays
spellingShingle	Auger Observatory Exposure Extensive air showers Trigger Ultra high energy cosmic rays Augers Cosmology Observatories Particle detectors Auger observatory Exposure Extensive air showers Trigger Ultra high-energy cosmic rays Cosmic rays Multitudinario:475 Trigger and aperture of the surface detector array of the Pierre Auger Observatory
topic_facet	Auger Observatory Exposure Extensive air showers Trigger Ultra high energy cosmic rays Augers Cosmology Observatories Particle detectors Auger observatory Exposure Extensive air showers Trigger Ultra high-energy cosmic rays Cosmic rays
description	The surface detector array of the Pierre Auger Observatory consists of 1600 water-Cherenkov detectors, for the study of extensive air showers (EAS) generated by ultra-high-energy cosmic rays. We describe the trigger hierarchy, from the identification of candidate showers at the level of a single detector, amongst a large background (mainly random single cosmic ray muons), up to the selection of real events and the rejection of random coincidences. Such trigger makes the surface detector array fully efficient for the detection of EAS with energy above 3 × 10 18 eV, for all zenith angles between 0 {ring operator} and 60 {ring operator} , independently of the position of the impact point and of the mass of the primary particle. In these range of energies and angles, the exposure of the surface array can be determined purely on the basis of the geometrical acceptance. © 2009 Elsevier B.V. All rights reserved.
format	JOUR
author	Multitudinario:475
author_facet	Multitudinario:475
author_sort	Multitudinario:475
title	Trigger and aperture of the surface detector array of the Pierre Auger Observatory
title_short	Trigger and aperture of the surface detector array of the Pierre Auger Observatory
title_full	Trigger and aperture of the surface detector array of the Pierre Auger Observatory
title_fullStr	Trigger and aperture of the surface detector array of the Pierre Auger Observatory
title_full_unstemmed	Trigger and aperture of the surface detector array of the Pierre Auger Observatory
title_sort	trigger and aperture of the surface detector array of the pierre auger observatory
url	http://hdl.handle.net/20.500.12110/paper_01689002_v613_n1_p29_Multitudinario
work_keys_str_mv	AT multitudinario475 triggerandapertureofthesurfacedetectorarrayofthepierreaugerobservatory
_version_	1807317978106036224

Trigger and aperture of the surface detector array of the Pierre Auger Observatory

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