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

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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Publicado:	2010
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:	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_01689002_v613_n1_p29_Multitudinario 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	paper:paper_01689002_v613_n1_p29_Multitudinario
record_format	dspace
spelling	paper:paper_01689002_v613_n1_p29_Multitudinario2023-06-08T15:18:02Z Trigger and aperture of the surface detector array of the Pierre Auger Observatory 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. 2010 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_01689002_v613_n1_p29_Multitudinario 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 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.
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
publishDate	2010
url	https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_01689002_v613_n1_p29_Multitudinario http://hdl.handle.net/20.500.12110/paper_01689002_v613_n1_p29_Multitudinario
_version_	1768546439891255296

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

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