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dc.contributor.authorAbeysekara, A. U.
dc.contributor.authorArcher, A.
dc.contributor.authorBenbow, W.
dc.contributor.authorBird, R.
dc.contributor.authorBrill, A.
dc.contributor.authorBrose, R.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorChristiansen, J. L.
dc.contributor.authorChromey, A. J.
dc.contributor.authorDaniel, M. K.
dc.contributor.authorFalcone, A.
dc.contributor.authorFeng, Q.
dc.contributor.authorFinley, J. P.
dc.contributor.authorFortson, L.
dc.contributor.authorFurniss, A.
dc.contributor.authorGillanders, G. H.
dc.contributor.authorGueta, O.
dc.contributor.authorHanna, D.
dc.contributor.authorHervet, O.
dc.contributor.authorHolder, J.
dc.contributor.authorHughes, G.
dc.contributor.authorHumensky, T. B.
dc.contributor.authorJohnson, C. A.
dc.contributor.authorKaaret, P.
dc.contributor.authorKar, P.
dc.contributor.authorKelley-Hoskins, N.
dc.contributor.authorKertzman, M.
dc.contributor.authorKieda, D.
dc.contributor.authorKrause, M.
dc.contributor.authorKrennrich, F.
dc.contributor.authorLang, M. J.
dc.contributor.authorMoriarty, P.
dc.contributor.authorMukherjee, R.
dc.contributor.authorO’Brien, S.
dc.contributor.authorOng, R. A.
dc.contributor.authorOtte, A. N.
dc.contributor.authorPark, N.
dc.contributor.authorPetrashyk, A.
dc.contributor.authorPohl, M.
dc.contributor.authorPueschel, E.
dc.contributor.authorQuinn, J.
dc.contributor.authorRagan, K.
dc.contributor.authorReynolds, P. T.
dc.contributor.authorRichards, G. T.
dc.contributor.authorRoache, E.
dc.contributor.authorRulten, C.
dc.contributor.authorSadeh, I.
dc.contributor.authorSantander, M.
dc.contributor.authorScott, S. S.
dc.contributor.authorSembroski, G. H.
dc.contributor.authorShahinyan, K.
dc.contributor.authorTyler, J.
dc.contributor.authorWakely, S. P.
dc.contributor.authorWeinstein, A.
dc.contributor.authorWells, R. M.
dc.contributor.authorWilcox, P.
dc.contributor.authorWilhelm, A.
dc.contributor.authorWilliams, D. A.
dc.contributor.authorWilliamson, T. J
dc.contributor.authorZitzer, B.
dc.contributor.authorKaur, A.
dc.contributor.author,
dc.date.accessioned2018-09-20T15:58:36Z
dc.date.available2018-09-20T15:58:36Z
dc.date.issued2018-07-12
dc.identifier.citationAbeysekara, A. U. Archer, A.; Benbow, W.; Bird, R.; Brill, A.; Brose, R.; Buckley, J. H.; Christiansen, J. L.; Chromey, A. J.; Daniel, M. K.; Falcone, A.; Feng, Q.; Finley, J. P.; Fortson, L.; Furniss, A.; Gillanders, G. H.; Gueta, O.; Hanna, D.; Hervet, O.; Holder, J.; Hughes, G.; Humensky, T. B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kelley-Hoskins, N.; Kertzman, M.; Kieda, D.; Krause, M.; Krennrich, F.; Lang, M. J.; Moriarty, P.; Mukherjee, R.; O’Brien, S.; Ong, R. A.; Otte, A. N.; Park, N.; Petrashyk, A.; Pohl, M.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Richards, G. T.; Roache, E.; Rulten, C.; Sadeh, I.; Santander, M.; Scott, S. S.; Sembroski, G. H.; Shahinyan, K.; Tyler, J.; Wakely, S. P.; Weinstein, A.; Wells, R. M.; Wilcox, P.; Wilhelm, A.; Williams, D. A.; Williamson, T. J; Zitzer, B.; Kaur, A.; , (2018). Veritas observations of the bl lac object txs 0506+056. The Astrophysical Journal 861 (2),
dc.identifier.issn2041-8213
dc.identifier.urihttp://hdl.handle.net/10379/10076
dc.description.abstractOn 2017 September 22, the IceCube Neutrino Observatory reported the detection of the high-energy neutrino event IC 170922A, of potential astrophysical origin. It was soon determined that the neutrino direction was consistent with the location of the gamma-ray blazar TXS 0506+056. (3FGL J0509.4+ 0541), which was in an elevated gamma-ray emission state as measured by the Fermi satellite. Very Energetic Radiation Imaging Telescope Array System (VERITAS) observations of the neutrino/blazar region started on 2017 September 23 in response to the neutrino alert and continued through 2018 February 6. While no significant very-high-energy (VHE; E > 100 GeV) emission was observed from the blazar by VERITAS in the two-week period immediately following the IceCube alert, TXS 0506+ 056 was detected by VERITAS with a significance of 5.8 standard deviations (sigma) in the full 35 hr data set. The average photon flux of the source during this period was (8.9 +/- 1.6). x. 10(-12) cm(-2) s(-1), or 1.6% of the Crab Nebula flux, above an energy threshold of 110 GeV, with a soft spectral index of 4.8. +/-. 1.3.
dc.publisherAmerican Astronomical Society
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.subjectastroparticle physics
dc.subjectbl lacertae objects: individual (txs 0506+056, ver j0509+057)
dc.subjectgamma rays: galaxies
dc.subjectquasars: general
dc.subjectneutrinos
dc.subjectactive galactic nuclei
dc.subjecttelescope
dc.subjectradiation
dc.subjectmission
dc.subjectblazar
dc.subjecti.
dc.titleVeritas observations of the bl lac object txs 0506+056
dc.typeArticle
dc.identifier.doi10.3847/2041-8213/aad053
dc.local.publishedsourcehttp://arxiv.org/pdf/1807.04607
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