Author/Authors :
Singh، نويسنده , , B.B. and Chitnis، نويسنده , , V.R. and Bose، نويسنده , , D. and Rahman، نويسنده , , M.A. and Upadhya، نويسنده , , S.S. and Gothe، نويسنده , , K.S. and Nagesh، نويسنده , , B.K. and Purohit، نويسنده , , P.N. Praveen Rao، نويسنده , , Shobha K. and Rao، نويسنده , , Kamesh K. and Sharma، نويسنده , , S.K. and Sudersan، نويسنده , , P.V. and Venkateshmurthy، نويسنده , , B.L. and Vishwanath، نويسنده , , P.R. and Acharya، نويسنده , , B.S.، نويسنده ,
Abstract :
We present the results of observation of the Geminga pulsar carried out in the TeV energy band during the 6 year period spanning 2000–2006 using the Pachmarhi Array of Cherenkov Telescopes (PACT). A long stretch of data, new computer codes and the “Tempo” package have been used in the present analysis. We have searched for evidence of pulsed emission of γ -rays from the Geminga pulsar using the post-glitch pulsar elements obtained by Jackson and Halpern from X-ray/ γ -ray satellite data. We do not see any significant evidence for pulsed emission from the Geminga pulsar at a threshold energy of 825 GeV. In this paper we present our results on the light curve in the TeV energy band, set an upper limit on the time averaged flux of γ -rays, and compare our results with other ground based observations.
Keywords :
TeV ? -rays , Atmospheric Cherenkov technique , Geminga pulsar , PACT
