Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory

We report a measurement of the flux of cosmic rays with unprecedented precision and Statistics using the Pierre Auger Observatory Based on fluorescence observations in coincidence with at least one Surface detector we derive a spectrum for energies above 10(18) eV We also update the previously publi...

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Detalhes bibliográficos
Autores: Arganda, E., Arqueros Martínez, Fernando, Blanco Ramos, Francisco, García Pinto, Diego, Monasor, M., Ortiz Ramis, Montserrat, Rosado Vélez, Jaime, Vázquez Peñas, José Ramón
Formato: artículo
Fecha de publicación:2010
País:España
Recursos:Universidad Complutense de Madrid (UCM)
Repositorio:Docta Complutense
Idioma:inglés
OAI Identifier:oai:docta.ucm.es:20.500.14352/45137
Acesso em linha:https://hdl.handle.net/20.500.14352/45137
Access Level:acceso abierto
Palavra-chave:539.1
Surface detector
Upper limit
Photon fraction
Simulation
Electrons
Showers
System
Array.
Física nuclear
2207 Física Atómica y Nuclear
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oai_identifier_str oai:docta.ucm.es:20.500.14352/45137
network_acronym_str ES
network_name_str España
repository_id_str
spelling Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger ObservatoryArganda, E.Arqueros Martínez, FernandoBlanco Ramos, FranciscoGarcía Pinto, DiegoMonasor, M.Ortiz Ramis, MontserratRosado Vélez, JaimeVázquez Peñas, José Ramón539.1Surface detectorUpper limitPhoton fractionSimulationElectronsShowersSystemArray.Física nuclear2207 Física Atómica y NuclearWe report a measurement of the flux of cosmic rays with unprecedented precision and Statistics using the Pierre Auger Observatory Based on fluorescence observations in coincidence with at least one Surface detector we derive a spectrum for energies above 10(18) eV We also update the previously published energy spectrum obtained with the surface detector array The two spectra are combined addressing the systematic uncertainties and, in particular. the influence of the energy resolution on the spectral shape The spectrum can be described by a broken power law E-gamma with index gamma = 3 3 below the ankle which is measured at log(10)(E-ankle/eV) = 18 6 Above the ankle the spectrum is described by a power law with index 2 6 followed by a flux suppression, above about log(10)(E/eV) = 19 5, detected with high statistical significance (C) 2010 Elsevier B V All rights reservedElsevier Science BVUniversidad Complutense de Madrid20102010-03-0820102010-03-08journal articlehttp://purl.org/coar/resource_type/c_6501info:eu-repo/semantics/articleapplication/pdfhttps://hdl.handle.net/20.500.14352/45137reponame:Docta Complutenseinstname:Universidad Complutense de Madrid (UCM)Inglésengopen accesshttp://purl.org/coar/access_right/c_abf2Atribución 3.0 Españahttps://creativecommons.org/licenses/by/3.0/es/info:eu-repo/semantics/openAccessoai:docta.ucm.es:20.500.14352/451372026-06-02T12:44:21Z
dc.title.none.fl_str_mv Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
title Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
spellingShingle Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
Arganda, E.
539.1
Surface detector
Upper limit
Photon fraction
Simulation
Electrons
Showers
System
Array.
Física nuclear
2207 Física Atómica y Nuclear
title_short Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
title_full Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
title_fullStr Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
title_full_unstemmed Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
title_sort Measurement of the energy spectrum of cosmic rays above 10(18) eV using the Pierre Auger Observatory
dc.creator.none.fl_str_mv Arganda, E.
Arqueros Martínez, Fernando
Blanco Ramos, Francisco
García Pinto, Diego
Monasor, M.
Ortiz Ramis, Montserrat
Rosado Vélez, Jaime
Vázquez Peñas, José Ramón
author Arganda, E.
author_facet Arganda, E.
Arqueros Martínez, Fernando
Blanco Ramos, Francisco
García Pinto, Diego
Monasor, M.
Ortiz Ramis, Montserrat
Rosado Vélez, Jaime
Vázquez Peñas, José Ramón
author_role author
author2 Arqueros Martínez, Fernando
Blanco Ramos, Francisco
García Pinto, Diego
Monasor, M.
Ortiz Ramis, Montserrat
Rosado Vélez, Jaime
Vázquez Peñas, José Ramón
author2_role author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Universidad Complutense de Madrid
dc.subject.none.fl_str_mv 539.1
Surface detector
Upper limit
Photon fraction
Simulation
Electrons
Showers
System
Array.
Física nuclear
2207 Física Atómica y Nuclear
topic 539.1
Surface detector
Upper limit
Photon fraction
Simulation
Electrons
Showers
System
Array.
Física nuclear
2207 Física Atómica y Nuclear
description We report a measurement of the flux of cosmic rays with unprecedented precision and Statistics using the Pierre Auger Observatory Based on fluorescence observations in coincidence with at least one Surface detector we derive a spectrum for energies above 10(18) eV We also update the previously published energy spectrum obtained with the surface detector array The two spectra are combined addressing the systematic uncertainties and, in particular. the influence of the energy resolution on the spectral shape The spectrum can be described by a broken power law E-gamma with index gamma = 3 3 below the ankle which is measured at log(10)(E-ankle/eV) = 18 6 Above the ankle the spectrum is described by a power law with index 2 6 followed by a flux suppression, above about log(10)(E/eV) = 19 5, detected with high statistical significance (C) 2010 Elsevier B V All rights reserved
publishDate 2010
dc.date.none.fl_str_mv 2010
2010-03-08
2010
2010-03-08
dc.type.none.fl_str_mv journal article
http://purl.org/coar/resource_type/c_6501
dc.type.openaire.fl_str_mv info:eu-repo/semantics/article
format article
dc.identifier.none.fl_str_mv https://hdl.handle.net/20.500.14352/45137
url https://hdl.handle.net/20.500.14352/45137
dc.language.none.fl_str_mv Inglés
eng
language_invalid_str_mv Inglés
language eng
dc.rights.none.fl_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución 3.0 España
https://creativecommons.org/licenses/by/3.0/es/
dc.rights.openaire.fl_str_mv info:eu-repo/semantics/openAccess
rights_invalid_str_mv open access
http://purl.org/coar/access_right/c_abf2
Atribución 3.0 España
https://creativecommons.org/licenses/by/3.0/es/
eu_rights_str_mv openAccess
dc.format.none.fl_str_mv application/pdf
dc.publisher.none.fl_str_mv Elsevier Science BV
publisher.none.fl_str_mv Elsevier Science BV
dc.source.none.fl_str_mv reponame:Docta Complutense
instname:Universidad Complutense de Madrid (UCM)
instname_str Universidad Complutense de Madrid (UCM)
reponame_str Docta Complutense
collection Docta Complutense
repository.name.fl_str_mv
repository.mail.fl_str_mv
_version_ 1869422578513215488
score 15.228081

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