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dc.contributor.authorDaniel, M. K.
dc.contributor.authorBadran, H. M.
dc.contributor.authorBond, I. H.
dc.contributor.authorBoyle, P. J.
dc.contributor.authorBradbury, S. M.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorCarter‐Lewis, D. A.
dc.contributor.authorCatanese, M.
dc.contributor.authorCelik, O.
dc.contributor.authorCogan, P.
dc.contributor.authorCui, W.
dc.contributor.authorD’Vali, M.
dc.contributor.authorde la Calle Perez, I.
dc.contributor.authorDuke, C.
dc.contributor.authorFalcone, A.
dc.contributor.authorFegan, D. J.
dc.contributor.authorFegan, S. J.
dc.contributor.authorFinley, J. P.
dc.contributor.authorFortson, L. F.
dc.contributor.authorGaidos, J. A.
dc.contributor.authorGammell, S.
dc.contributor.authorGibbs, K.
dc.contributor.authorGillanders, G. H.
dc.contributor.authorGrube, J.
dc.contributor.authorHall, J.
dc.contributor.authorHall, T. A.
dc.contributor.authorHanna, D.
dc.contributor.authorHillas, A. M.
dc.contributor.authorHolder, J.
dc.contributor.authorHoran, D.
dc.contributor.authorHumensky, T. B.
dc.contributor.authorJarvis, A.
dc.contributor.authorJordan, M.
dc.contributor.authorKenny, G. E.
dc.contributor.authorKertzman, M.
dc.contributor.authorKieda, D.
dc.contributor.authorKildea, J.
dc.contributor.authorKnapp, J.
dc.contributor.authorKosack, K.
dc.contributor.authorKrawczynski, H.
dc.contributor.authorKrennrich, F.
dc.contributor.authorLang, M. J.
dc.contributor.authorLe Bohec, S.
dc.contributor.authorLinton, E.
dc.contributor.authorLloyd‐Evans, J.
dc.contributor.authorMilovanovic, A.
dc.contributor.authorMoriarty, P.
dc.contributor.authorMuller, D.
dc.contributor.authorNagai, T.
dc.contributor.authorNolan, S.
dc.contributor.authorOng, R. A.
dc.contributor.authorPallassini, R.
dc.contributor.authorPetry, D.
dc.contributor.authorPower‐Mooney, B.
dc.contributor.authorQuinn, J.
dc.contributor.authorQuinn, M.
dc.contributor.authorRagan, K.
dc.contributor.authorRebillot, P.
dc.contributor.authorReynolds, P. T.
dc.contributor.authorRose, H. J.
dc.contributor.authorSchroedter, M.
dc.contributor.authorSembroski, G. H.
dc.contributor.authorSwordy, S. P.
dc.contributor.authorSyson, A.
dc.contributor.authorVassiliev, V. V.
dc.contributor.authorWakely, S. P.
dc.contributor.authorWalker, G.
dc.contributor.authorWeekes, T. C.
dc.contributor.authorZweerink, J.
dc.identifier.citationDaniel, M. K. Badran, H. M.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Buckley, J. H.; Carter‐Lewis, D. A.; Catanese, M.; Celik, O.; Cogan, P.; Cui, W.; D’Vali, M.; de la Calle Perez, I.; Duke, C.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Fortson, L. F.; Gaidos, J. A.; Gammell, S.; Gibbs, K.; Gillanders, G. H.; Grube, J.; Hall, J.; Hall, T. A.; Hanna, D.; Hillas, A. M.; Holder, J.; Horan, D.; Humensky, T. B.; Jarvis, A.; Jordan, M.; Kenny, G. E.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Le Bohec, S.; Linton, E.; Lloyd‐Evans, J.; Milovanovic, A.; Moriarty, P.; Muller, D.; Nagai, T.; Nolan, S.; Ong, R. A.; Pallassini, R.; Petry, D.; Power‐Mooney, B.; Quinn, J.; Quinn, M.; Ragan, K.; Rebillot, P.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Swordy, S. P.; Syson, A.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.; Zweerink, J. (2005). Spectrum of very high energy gamma‐rays from the blazar 1es 1959+650 during flaring activity in 2002. The Astrophysical Journal 621 (1), 181-187
dc.description.abstractThe blazar 1ES 1959+650 was observed in a flaring state with the Whipple 10 m Imaging Atmospheric Cerenkov Telescope in 2002 May. A spectral analysis has been carried out on the data from that time period, and the resulting very high energy gamma-ray spectrum (E greater than or equal to 316 GeV) can be well fitted by a power law of differential spectral index alpha = 2.78 +/- 0.12(stat) +/- 0.21(sys). On 2002 June 4, the source flared dramatically in the gamma-ray range without any coincident increase in the X-ray emission, providing the first unambiguous example of an "orphan'' gamma-ray flare from a blazar. The gamma-ray spectrum for these data can also be described by a simple power-law fit with alpha = 2.82 +/- 0.15(stat) +/- 0.30(sys). There is no compelling evidence for spectral variability or for any cutoff to the spectrum.
dc.publisherIOP Publishing
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Ireland
dc.subjectbl lacertae objects : individual (1es 1959+650)
dc.subjectgamma rays : observations
dc.subjecttechniques : spectroscopic
dc.subjectcherenkov telescopes
dc.subjectstrong flares
dc.subjecttev energies
dc.titleSpectrum of very high energy gamma‐rays from the blazar 1es 1959+650 during flaring activity in 2002

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