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https://hdl.handle.net/2440/12600
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DC Field | Value | Language |
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dc.contributor.author | Roberts, M. D. | en |
dc.contributor.author | Edwards, Philip Gregory | en |
dc.contributor.author | Patterson, J. R. | en |
dc.contributor.author | Thornton, G. J. | en |
dc.contributor.author | Meyhandan, Rishi | en |
dc.date.issued | 1998 | en |
dc.identifier.citation | Journal of Physics G: Nuclear Particle Physics, 1998; 24(1):255-266 | en |
dc.identifier.issn | 0954-3899 | en |
dc.identifier.uri | http://hdl.handle.net/2440/12600 | - |
dc.description.abstract | Very high energy gamma-ray astronomers using the atmospheric Cerenkov technique must contend with a large background of light pulses due to cosmic ray-initiated cascades. Significant advances have been made in developing techniques to reduce this background: the imaging technique can have a figure of merit, q, in excess of 6 near the zenith. However, q decreases as the zenith angle increases. In this paper we describe a new technique based on the temporal Cerenkov pulse shape and show that the use of rise time and FWHM cuts are effective discriminators at all zenith angles. For flat-spectrum sources at large zenith angles q ~ 2.5. Measured parameter distributions are compared with simulations and the methods of making the cuts are discussed. A sensitivity to cosmic-ray composition is also suggested. | en |
dc.description.statementofresponsibility | M D Roberts, P G Edwards, J R Patterson, G J Thornton and R Meyhandan | en |
dc.language.iso | en | en |
dc.title | Pulse shape selection in very high energy gamma-ray astronomy | en |
dc.type | Journal article | en |
dc.identifier.doi | 10.1088/0954-3899/24/1/027 | en |
Appears in Collections: | Physics publications |
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