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Discovery of tev gamma-ray emission toward supernova remnant snr g78.2+2.1

dc.contributor.authorAliu, E.
dc.contributor.authorArchambault, S.
dc.contributor.authorArlen, T.
dc.contributor.authorAune, T.
dc.contributor.authorBeilicke, M.
dc.contributor.authorBenbow, W.
dc.contributor.authorBird, R.
dc.contributor.authorBouvier, A.
dc.contributor.authorBradbury, S. M.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorBugaev, V.
dc.contributor.authorByrum, K.
dc.contributor.authorCannon, A.
dc.contributor.authorCesarini, A.
dc.contributor.authorCiupik, L.
dc.contributor.authorCollins-Hughes, E.
dc.contributor.authorConnolly, M. P.
dc.contributor.authorCui, W.
dc.contributor.authorDickherber, R.
dc.contributor.authorDuke, C.
dc.contributor.authorDumm, J.
dc.contributor.authorDwarkadas, V. V.
dc.contributor.authorErrando, M.
dc.contributor.authorFalcone, A.
dc.contributor.authorFederici, S.
dc.contributor.authorFeng, Q.
dc.contributor.authorFinley, J. P.
dc.contributor.authorFinnegan, G.
dc.contributor.authorFortson, L.
dc.contributor.authorFurniss, A.
dc.contributor.authorGalante, N.
dc.contributor.authorGall, D.
dc.contributor.authorGillanders, G. H.
dc.contributor.authorGodambe, S.
dc.contributor.authorGotthelf, E. V.
dc.contributor.authorGriffin, S.
dc.contributor.authorGrube, J.
dc.contributor.authorGyuk, G.
dc.contributor.authorHanna, D.
dc.contributor.authorHolder, J.
dc.contributor.authorHuan, H.
dc.contributor.authorHughes, G.
dc.contributor.authorHumensky, T. B.
dc.contributor.authorKaaret, P.
dc.contributor.authorKarlsson, N.
dc.contributor.authorKertzman, M.
dc.contributor.authorKhassen, Y.
dc.contributor.authorKieda, D.
dc.contributor.authorKrawczynski, H.
dc.contributor.authorKrennrich, F.
dc.contributor.authorLang, M. J.
dc.contributor.authorLee, K.
dc.contributor.authorMadhavan, A. S
dc.contributor.authorMaier, G.
dc.contributor.authorMajumdar, P.
dc.contributor.authorMcArthur, S.
dc.contributor.authorMcCann, A.
dc.contributor.authorMillis, J.
dc.contributor.authorMoriarty, P.
dc.contributor.authorMukherjee, R.
dc.contributor.authorNelson, T.
dc.contributor.authorO'Faoláin de Bhróithe, A.
dc.contributor.authorOng, R. A.
dc.contributor.authorOrr, M.
dc.contributor.authorOtte, A. N.
dc.contributor.authorPandel, D.
dc.contributor.authorPark, N.
dc.contributor.authorPerkins, J. S.
dc.contributor.authorPohl, M.
dc.contributor.authorPopkow, A.
dc.contributor.authorProkoph, H.
dc.contributor.authorQuinn, J.
dc.contributor.authorRagan, K.
dc.contributor.authorReyes, L. C.
dc.contributor.authorReynolds, P. T.
dc.contributor.authorRoache, E.
dc.contributor.authorRose, H. J.
dc.contributor.authorRuppel, J.
dc.contributor.authorSaxon, D. B.
dc.contributor.authorSchroedter, M.
dc.contributor.authorSembroski, G. H.
dc.contributor.authorŞentürk, G. D.
dc.contributor.authorSkole, C.
dc.contributor.authorTelezhinsky, I.
dc.contributor.authorTešić, G.
dc.contributor.authorTheiling, M.
dc.contributor.authorThibadeau, S.
dc.contributor.authorTsurusaki, K.
dc.contributor.authorTyler, J.
dc.contributor.authorVarlotta, A.
dc.contributor.authorVassiliev, V. V.
dc.contributor.authorVincent, S.
dc.contributor.authorWakely, S. P.
dc.contributor.authorWard, J. E.
dc.contributor.authorWeekes, T. C.
dc.contributor.authorWeinstein, A.
dc.contributor.authorWeisgarber, T.
dc.contributor.authorWelsing, R.
dc.contributor.authorWilliams, D. A.
dc.contributor.authorZitzer, B.
dc.date.accessioned2018-09-20T15:59:27Z
dc.date.available2018-09-20T15:59:27Z
dc.date.issued2013-05-29
dc.identifier.citationAliu, E. Archambault, S.; Arlen, T.; Aune, T.; Beilicke, M.; Benbow, W.; Bird, R.; Bouvier, A.; Bradbury, S. M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cannon, A.; Cesarini, A.; Ciupik, L.; Collins-Hughes, E.; Connolly, M. P.; Cui, W.; Dickherber, R.; Duke, C.; Dumm, J.; Dwarkadas, V. V.; Errando, M.; Falcone, A.; Federici, S.; Feng, Q.; Finley, J. P.; Finnegan, G.; Fortson, L.; Furniss, A.; Galante, N.; Gall, D.; Gillanders, G. H.; Godambe, S.; Gotthelf, E. V.; Griffin, S.; Grube, J.; Gyuk, G.; Hanna, D.; Holder, J.; Huan, H.; Hughes, G.; Humensky, T. B.; Kaaret, P.; Karlsson, N.; Kertzman, M.; Khassen, Y.; Kieda, D.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Lee, K.; Madhavan, A. S; Maier, G.; Majumdar, P.; McArthur, S.; McCann, A.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nelson, T.; O'Faoláin de Bhróithe, A.; Ong, R. A.; Orr, M.; Otte, A. N.; Pandel, D.; Park, N.; Perkins, J. S.; Pohl, M.; Popkow, A.; Prokoph, H.; Quinn, J.; Ragan, K.; Reyes, L. C.; Reynolds, P. T.; Roache, E.; Rose, H. J.; Ruppel, J.; Saxon, D. B.; Schroedter, M.; Sembroski, G. H.; Şentürk, G. D.; Skole, C.; Telezhinsky, I.; Tešić, G.; Theiling, M.; Thibadeau, S.; Tsurusaki, K.; Tyler, J.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Ward, J. E.; Weekes, T. C.; Weinstein, A.; Weisgarber, T.; Welsing, R.; Williams, D. A.; Zitzer, B. (2013). Discovery of tev gamma-ray emission toward supernova remnant snr g78.2+2.1. The Astrophysical Journal 770 (2),
dc.identifier.issn0004-637X,1538-4357
dc.identifier.urihttp://hdl.handle.net/10379/10199
dc.description.abstractWe report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0 degrees.23 +/- 0 degrees.03(stat-0 degrees.02sys)(+0 degrees.04) and its spectrum is well-characterized by a differential power law (dN/dE = N-0 x (E/TeV)-Gamma) with a photon index of Gamma = 2.37 +/- 0.14(stat) +/- 0.20(sys) and a flux normalization of N-0 = 1.5 +/- 0.2(stat) +/- 0.4(sys) x 10(-12) photon TeV-1 cm(-2) s(-1). This yields an integral flux of 5.2 +/- 0.8(stat) +/- 1.4(sys) x 10(-12) photon cm(-2) s(-1) above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the SNR shock.
dc.publisherIOP Publishing
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Ireland
dc.rights.urihttps://creativecommons.org/licenses/by-nc-nd/3.0/ie/
dc.subjectacceleration of particles
dc.subjectcosmic rays
dc.subjectgamma rays: general
dc.subjectism: supernova remnants
dc.subjectparticle-acceleration
dc.subjectfermi
dc.subjecthess
dc.subjectsearch
dc.subjectcounterpart
dc.subject2cg078+2
dc.subjectcatalog
dc.subjectorigin
dc.titleDiscovery of tev gamma-ray emission toward supernova remnant snr g78.2+2.1
dc.typeArticle
dc.identifier.doi10.1088/0004-637x/770/2/93
dc.local.publishedsourcehttp://iopscience.iop.org/article/10.1088/0004-637X/770/2/93/pdf
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