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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4562
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dc.contributor.authorSripathi Acharya, B-
dc.contributor.authorVishwanath, P. R-
dc.contributor.authorBhat, P. N-
dc.contributor.authorChitnis, V. R-
dc.contributor.authorMajumdar, P-
dc.contributor.authorRahman, M. A-
dc.contributor.authorSingh, B. B-
dc.date.accessioned2009-06-17T16:57:15Z-
dc.date.available2009-06-17T16:57:15Z-
dc.date.issued2003-07-
dc.identifier.citationKajita, Y. Asaoka, A. Kawachi, Y. Matsubara and M. Sasaki., eds., Proceedings of the 28th International Cosmic Ray Conference. July 31 - August 7, Trukuba, Japan, 2003. pp. 2501 - 2504en
dc.identifier.isbn4-946443-80-0-
dc.identifier.urihttp://hdl.handle.net/2248/4562-
dc.description.abstractThe data taken on the Crab pulsar by the recently commissioned array of ˇ Cerenkov telescopes at Pachmarhi using the wave front sampling technique have been analyzed. The phasograms show significant excess of events at the Radio Main Pulse phase. This excess corresp onds to a 5.7σ signal and is confined to a narrow angular region around the source. It is present in most runs indicating constancy of emission. The energy estimate of the events indicate that the signal is due to higher energy events. This excess could corresp ond to the possible second component of Outer Gap models.en
dc.language.isoenen
dc.publisherInternational Union of Pure and Applied Physicsen
dc.relation.urihttp://adsabs.harvard.edu/abs/2003ICRC....4.2501Sen
dc.subjectPACT Resultsen
dc.subjectVery High Energy g-Ray Emissionen
dc.subjectCRAB Pulsaren
dc.subjectRadio Main Pulse Phaseen
dc.titlePACT results on very high energy g-ray emission from CRAB pulsaren
dc.typeArticleen
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