Author/Authors :
Ahrens، نويسنده , , J. and Bai، نويسنده , , X. and Bay، نويسنده , , R. S. Barwick، نويسنده , , S.W. and Becka، نويسنده , , T. and Becker، نويسنده , , J.K. and Becker، نويسنده , , K.-H. and Bernardini، نويسنده , , E. and Bertrand، نويسنده , , D. and Biron، نويسنده , , A. and Boersma، نويسنده , , D.J. and B?ser، نويسنده , , S. and Botner، نويسنده , , O. and Bouchta، نويسنده , , A. and Bouhali، نويسنده , , O. and Burgess، نويسنده , , T. and Cari، نويسنده ,
Abstract :
The Antarctic Muon And Neutrino Detector Array (AMANDA) is a high-energy neutrino telescope operating at the geographic South Pole. It is a lattice of photo-multiplier tubes buried deep in the polar ice between 1500 and 2000 m. The primary goal of this detector is to discover astrophysical sources of high-energy neutrinos. A high-energy muon neutrino coming through the earth from the Northern Hemisphere can be identified by the secondary muon moving upward through the detector.
on tracks are reconstructed with a maximum likelihood method. It models the arrival times and amplitudes of Cherenkov photons registered by the photo-multipliers. This paper describes the different methods of reconstruction, which have been successfully implemented within AMANDA. Strategies for optimizing the reconstruction performance and rejecting background are presented. For a typical analysis procedure the direction of tracks are reconstructed with about 2° accuracy.
Keywords :
AMANDA , Neutrino telescope , Track reconstruction , Neutrino astrophysics
