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dc.contributor.authorKrennrich, F.
dc.contributor.authorBiller, S. D.
dc.contributor.authorBond, I. H.
dc.contributor.authorBoyle, P. J.
dc.contributor.authorBradbury, S. M.
dc.contributor.authorBreslin, A. C.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorBurdett, A. M.
dc.contributor.authorGordo, J. Bussons
dc.contributor.authorCarter‐Lewis, D. A.
dc.contributor.authorCatanese, M.
dc.contributor.authorCawley, M. F.
dc.contributor.authorFegan, D. J.
dc.contributor.authorFinley, J. P.
dc.contributor.authorGaidos, J. A.
dc.contributor.authorHall, T.
dc.contributor.authorHillas, A. M.
dc.contributor.authorLamb, R. C.
dc.contributor.authorLessard, R. W.
dc.contributor.authorMasterson, C.
dc.contributor.authorMcEnery, J. E.
dc.contributor.authorMohanty, G.
dc.contributor.authorMoriarty, P.
dc.contributor.authorQuinn, J.
dc.contributor.authorRodgers, A. J.
dc.contributor.authorRose, H. J.
dc.contributor.authorSamuelson, F. W.
dc.contributor.authorSembroski, G. H.
dc.contributor.authorSrinivasan, R.
dc.contributor.authorVassiliev, V. V.
dc.contributor.authorWeekes, T. C.
dc.date.accessioned2018-08-24T08:25:22Z
dc.date.available2018-08-24T08:25:22Z
dc.date.issued1999-01-20
dc.identifier.citationKrennrich, F. Biller, S. D.; Bond, I. H.; Boyle, P. J.; Bradbury, S. M.; Breslin, A. C.; Buckley, J. H.; Burdett, A. M.; Gordo, J. Bussons; Carter‐Lewis, D. A.; Catanese, M.; Cawley, M. F.; Fegan, D. J.; Finley, J. P.; Gaidos, J. A.; Hall, T.; Hillas, A. M.; Lamb, R. C.; Lessard, R. W.; Masterson, C.; McEnery, J. E.; Mohanty, G.; Moriarty, P.; Quinn, J.; Rodgers, A. J.; Rose, H. J.; Samuelson, F. W.; Sembroski, G. H.; Srinivasan, R.; Vassiliev, V. V.; Weekes, T. C. (1999). Measurement of the multi‐tev gamma‐ray flare spectra of markarian 421 and markarian 501. The Astrophysical Journal 511 (1), 149-156
dc.identifier.issn0004-637X,1538-4357
dc.identifier.urihttp://hdl.handle.net/10379/9413
dc.description.abstractThe energy spectrum of Markarian 421 in flaring states has been measured from 0.3 to 10 TeV using both small and large zenith angle observations with the Whipple Observatory 10 m imaging telescope. The large zenith angle technique is useful for extending spectra to high energies, and the extraction of spectra with this technique is discussed. The resulting spectrum of Markarian 421 is fitted reasonably well by a simple power law: J(E)= E-2.54+/-0.03+/-0.10 photons m(-1) s(-1) TeV-1, where the first set of errors is statistical and the second set is systematic. This is in contrast to our recently reported spectrum of Markarian 501, which over a similar energy range has substantial curvature. The differences in TeV energy spectra of gamma-ray blazars reflect both the physics of the gamma-ray production mechanism and possibly differential absorption effects at the source or in the intergalactic medium. Since Markarian 421 and Markarian 501 have almost the same redshift (0.031 and 0.033, respectively), the difference in their energy spectra must be intrinsic to the sources and not due to intergalactic absorption, assuming the intergalactic infrared background is uniform.
dc.publisherIOP Publishing
dc.relation.ispartofThe Astrophysical Journal
dc.subjectbl lacertae objects : individual (markarian 421, markarian 501)
dc.subjectgalaxies : active
dc.subjectgamma rays : observations
dc.subjectactive galaxy markarian-421
dc.subjectradiation
dc.subjectphotons
dc.titleMeasurement of the multi‐tev gamma‐ray flare spectra of markarian 421 and markarian 501
dc.typeArticle
dc.identifier.doi10.1086/306677
dc.local.publishedsourcehttp://iopscience.iop.org/article/10.1086/306677/pdf
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