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dc.contributor.authorAbeysekara, A. U.
dc.contributor.authorArcher, A.
dc.contributor.authorBenbow, W.
dc.contributor.authorBird, R.
dc.contributor.authorBrose, R.
dc.contributor.authorBuchovecky, M.
dc.contributor.authorBugaev, V.
dc.contributor.authorConnolly, M. P.
dc.contributor.authorCui, W.
dc.contributor.authorErrando, M.
dc.contributor.authorFalcone, A.
dc.contributor.authorFeng, Q.
dc.contributor.authorFinley, J. P.
dc.contributor.authorFlinders, A.
dc.contributor.authorFortson, L.
dc.contributor.authorFurniss, A.
dc.contributor.authorGillanders, G. H.
dc.contributor.authorHütten, M.
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.authorLin, T. T. Y.
dc.contributor.authorMaier, G.
dc.contributor.authorMcArthur, S.
dc.contributor.authorMoriarty, P.
dc.contributor.authorMukherjee, R.
dc.contributor.authorO’Brien, S.
dc.contributor.authorOng, R. A.
dc.contributor.authorPark, N.
dc.contributor.authorPerkins, J. S.
dc.contributor.authorPetrashyk, A.
dc.contributor.authorPohl, M.
dc.contributor.authorPopkow, A.
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.authorSembroski, G. H.
dc.contributor.authorShahinyan, K.
dc.contributor.authorTyler, J.
dc.contributor.authorWakely, S. P.
dc.contributor.authorWeiner, O. M.
dc.contributor.authorWeinstein, A.
dc.contributor.authorWells, R. M.
dc.contributor.authorWilcox, P.
dc.contributor.authorWilhelm, A.
dc.contributor.authorWilliams, D. A.
dc.contributor.authorZitzer, B.
dc.contributor.authorVurm, Indrek
dc.contributor.authorBeloborodov, Andrei,
dc.identifier.citationAbeysekara, A. U. Archer, A.; Benbow, W.; Bird, R.; Brose, R.; Buchovecky, M.; Bugaev, V.; Connolly, M. P.; Cui, W.; Errando, M.; Falcone, A.; Feng, Q.; Finley, J. P.; Flinders, A.; Fortson, L.; Furniss, A.; Gillanders, G. H.; Hütten, M.; 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.; Lin, T. T. Y.; Maier, G.; McArthur, S.; Moriarty, P.; Mukherjee, R.; O’Brien, S.; Ong, R. A.; Park, N.; Perkins, J. S.; Petrashyk, A.; Pohl, M.; Popkow, A.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Richards, G. T.; Roache, E.; Rulten, C.; Sadeh, I.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Tyler, J.; Wakely, S. P.; Weiner, O. M.; Weinstein, A.; Wells, R. M.; Wilcox, P.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; Vurm, Indrek; Beloborodov, Andrei; , (2018). A strong limit on the very-high-energy emission from grb 150323a. The Astrophysical Journal 857 (1),
dc.description.abstractOn 2015 March 23, the Very Energetic Radiation Imaging Telescope Array System (VERITAS) responded to a Swift-Burst Alert Telescope (BAT) detection of a gamma-ray burst, with observations beginning 270 s after the onset of BAT emission, and only 135 s after the main BAT emission peak. No statistically significant signal is detected above 140 GeV. The VERITAS upper limit on the fluence in a 40-minute integration corresponds to about 1% of the prompt fluence. Our limit is particularly significant because the very-high-energy (VHE) observation started only similar to 2 minutes after the prompt emission peaked, and Fermi-Large Area Telescope observations of numerous other bursts have revealed that the high-energy emission is typically delayed relative to the prompt radiation and lasts significantly longer. Also, the proximity of GRB 150323A (z = 0.593) limits the attenuation by the extragalactic background light to similar to 50% at 100-200 GeV. We conclude that GRB 150323A had an intrinsically very weak high-energy afterglow, or that the GeV spectrum had a turnover below similar to 100 GeV. If the GRB exploded into the stellar wind of a massive progenitor, the VHE non-detection constrains the wind density parameter to be A greater than or similar to 3 x 10(11) g . cm(-1), consistent with a standard Wolf-Rayet progenitor. Alternatively, the VHE emission from the blast wave would be weak in a very tenuous medium such as the interstellar medium, which therefore cannot be ruled out as the environment of GRB 150323A.
dc.publisherAmerican Astronomical Society
dc.relation.ispartofThe Astrophysical Journal
dc.rightsAttribution-NonCommercial-NoDerivs 3.0 Ireland
dc.subjectgamma rays: general
dc.subjectgamma-ray burst: general
dc.subjectgamma-ray burst: individual (grb 150323a)
dc.subjectgamma-ray bursts
dc.subjectextragalactic background light
dc.titleA strong limit on the very-high-energy emission from grb 150323a

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