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dc.creatorAraya Arguedas, Miguel
dc.creatorMitchell, Alison M. W.
dc.creatorParsons, R. Daniel
dc.date.accessioned2023-12-06T20:57:18Z
dc.date.available2023-12-06T20:57:18Z
dc.date.issued2019-02-17
dc.identifier.citationhttps://academic.oup.com/mnras/article/485/1/1001/5322176es_ES
dc.identifier.issn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://hdl.handle.net/10669/90562
dc.description.abstractHESS J1825–137 is a bright very high-energy gamma-ray source that has been firmly established as a pulsar wind nebula (PWN), and one of the most extended gamma-ray objects within this category. The progenitor supernova remnant (SNR) for this PWN has not been firmly established. We carried out an analysis of gamma-ray observations in the region of HESS J1825–137 with the Fermi–LAT that reveals emission in the direction away from the Galactic plane.  The region lies beyond the PWN and reaches a distance from the pulsar compatible with the supposed location of the SNR shock front. The spectrum of the gamma-rays is hard with a photon index of ∼1.9 in the 10–250 GeV range. Several scenarios for the origin of the emission are discussed, including the SNR as a source of high-energy particles and the ‘leakage’ of leptons from the PWN.es_ES
dc.language.isoenges_ES
dc.sourceMonthly Notices of the Royal Astronomical Society, vol.485(1), pp. 1001–1007es_ES
dc.subjectISM individual objectses_ES
dc.subjectHESS J1825-137Aes_ES
dc.subjectISM supernova remnantses_ES
dc.subjectGamma rayses_ES
dc.titleRevealing a new region of gamma-ray emission in the vicinity of HESS J1825–137es_ES
dc.typeartículo originales_ES
dc.identifier.doi10.1093/mnras/stz462
dc.description.procedenceUCR::Vicerrectoría de Investigación::Unidades de Investigación::Ciencias Básicas::Centro de Investigaciones Espaciales (CINESPA)es_ES
dc.description.procedenceUCR::Vicerrectoría de Docencia::Ciencias Básicas::Facultad de Ciencias::Escuela de Físicaes_ES


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