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dc.contributor.authorSierpowska-Bartosik, Agnieszka-
dc.contributor.authorTorres, Diego F.-
dc.date.accessioned2008-06-29T14:33:31Z-
dc.date.available2008-06-29T14:33:31Z-
dc.date.issued2008-01-22-
dc.identifier.citationThe Astrophysical Journal Letters 674(2): L89-L92 (2008)en_US
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10261/5430-
dc.description4 pages.-- Printed version published on Feb 20, 2008.en_US
dc.description.abstractLS 5039 is one of a handful of X-ray binaries that have been recently detected at high-energy γ-rays, in this case, by the High Energy Stereoscopic System (H.E.S.S.). The nature of this system is unknown: both a black hole and a pulsar have been invoked as possible compact object companions. Here we work with a model of the high-energy phenomenology of the system in which it is assumed that the companion object is a pulsar rotating around an O6.5 V star in a ~3.9 day orbit. The model assumes two different sets of power-law spectral parameters of the interacting primary leptons corresponding to the two orbital phase intervals defined by H.E.S.S. as having different γ-ray spectra and very high energy (VHE) cutoffs. We show that the H.E.S.S. phenomenology is completely explained by this model. We present predictions for photons with lower energies (for E > 1 GeV), subject to test in the forthcoming months with the GLAST satellite. We find that GLAST will be able to judge on this model within 1 year.en_US
dc.description.sponsorshipWe acknowledge support by grants MEC-AYA 2006-00530 and CSIC-PIE 200750I029.en_US
dc.format.extent680827 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherAmerican Astronomical Society-
dc.publisherUniversity of Chicago Press-
dc.rightsopenAccessen_US
dc.subjectX-ray binaries (individual LS 5039)en_US
dc.subjectγ-rays: observationsen_US
dc.subjectγ-rays: theoryen_US
dc.subjectHigh-Energy Stereoscopy Array (H.E.S.S.) Telescopeen_US
dc.titleGLAST testing of a pulsar model matching H.E.S.S. observations of LS 5039en_US
dc.typeArtículoen_US
dc.identifier.doi10.1086/529376-
dc.description.peerreviewedPeer revieweden_US
dc.relation.publisherversionhttp://dx.doi.org/10.1086/529376-
dc.identifier.e-issn1538-4357-
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