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dc.contributor.authorLang, Mark
dc.contributor.authorGillanders, Gary
dc.contributor.authorLessard, R. W.
dc.contributor.authorBond, I. H.
dc.contributor.authorBradbury, S. M.
dc.contributor.authorBuckley, J. H.
dc.contributor.authorBurdett, A. M.
dc.contributor.authorCarter-Lewis, D. A.
dc.contributor.authorCatanese, M.
dc.contributor.authorCawley, M. F.
dc.contributor.authorD'Vali, M.
dc.contributor.authorFegan, D. J.
dc.contributor.authorFinley, J. P.
dc.contributor.authorGaidos, J. A.
dc.contributor.authorGillanders, G. H.
dc.contributor.authorHall, T.
dc.contributor.authorHillas, A. M.
dc.contributor.authorKrennrich, F.
dc.contributor.authorLang, M. J.
dc.contributor.authorMasterson, C.
dc.contributor.authorMoriarty, P.
dc.contributor.authorQuinn, 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.accessioned2012-01-20T10:31:21Z
dc.date.available2012-01-20T10:31:21Z
dc.date.issued1999
dc.identifier.urihttp://hdl.handle.net/10379/2489
dc.description.abstractWe present the results of a search for pulsed TeV emission from the Crab pulsar using the Whipple Observatory's 10 m gamma-ray telescope. The direction of the Crab pulsar was observed for a total of 73.4 hours between 1994 November and 1997 March. During this period the Whipple 10 m telescope was operated at its lowest energy threshold to date. Spectral analysis techniques were applied to search for the presence of a gamma-ray signal from the Crab pulsar over the energy band 250 GeV to 4 TeV. We do not see any evidence of the 33 ms pulsations present in other energy bands from the Crab pulsar. The 99.9% confidence level upper limit for pulsed emission above 250 GeV is derived to be 4.8x10^-12 cm^-2 s^-1 or <3% of the steady flux from the Crab Nebula. These results imply a sharp cut-off of the power-law spectrum seen by the EGRET instrument on the Compton Gamma-Ray Observatory. If the cut-off is exponential, it must begin at 60 GeV or lower to accommodate these upper limits.en_US
dc.formatapplication/pdfen_US
dc.language.isoenen_US
dc.subjectAstrophysicsen_US
dc.subjectPhysicsen_US
dc.titleSearch for Pulsed TeV Gamma-ray Emission from the Crab Pulsaren_US
dc.typeArticleen_US
dc.local.publishedsourcehttp://arxiv.org/pdf/astro-ph/9912520en_US
dc.description.peer-reviewedpeer-revieweden_US
dc.local.authorsR.W. Lessard, I.H. Bond, S.M. Bradbury, J.H. Buckley, A.M. Burdett, D.A. Carter-Lewis, M. Catanese, M.F. Cawley, M. D'Vali, D.J. Fegan, J.P. Finley, J.A. Gaidos, G.H. Gillanders, T. Hall, A.M. Hillas, F. Krennrich, M.J. Lang, C. Masterson, P. Moriarty, J. Quinn, H.J. Rose, F.W. Samuelson, G.H. Sembroski, R. Srinivasan, V.V. Vassiliev and T.C. Weekes
dc.local.arxividastro-ph/9912520
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