The AMANDA Neutrino Telescope and the Indirect Search for Dark Matter

A. Biron; A. Bouchta; A. Goobar; A. Hallgren; A. Jones; A. Karle; C. G. S. Costa; C. H. Wiebusch; C. P. De Los Heros; C. Spiering; C. Walck; D. Cowen; D. Lowder; D. Nygren; D. Potter; E. C. Andr&apos; E. Dalberg; E. Schneider; F. Halzen; For The Amanda Collaboration; Francis Halzen For; G. Hill; G. Yodh; H. Rubinstein; I. Liubarsky; J. Booth; J. Jacobsen; K. Woschnagg; L. Bergstrom; L. Gray; M. Carlson; M. Leuthold; M. Solarz; O. Streicher; P. Askebjer; P. B. Price; P. C. Mock; P. Ekstrom; P. Lindahl; P. Marciniewski; P. Miocinovic; P. Niessen; P. O. Hulth; R. C. Bay; R. Hardtke; R. Morse; R. Porrata; R. Schwarz; R. Wischnewski; S. Carius; S. Hart; S. Hundertmark; S. Tilav; S. W. Barwick; T. C. Miller; T. Deyoung; T. Thon; V. Kankhadai; Y. He

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The AMANDA Neutrino Telescope and the Indirect Search for Dark Matter

Abstract

With an effective telescope area of order 10^4 m^2, a threshold of ~50 GeV and a pointing accuracy of 2.5 degrees, the AMANDA detector represents the first of a new generation of high energy neutrino telescopes, reaching a scale envisaged over 25 years ago. We describe its performance, focussing on the capability to detect halo dark matter particles via their annihilation into neutrinos.Comment: Latex2.09, 16 pages, uses epsf.sty to place 15 postscript figures. Talk presented at the 3rd International Symposium on Sources and Detection of Dark Matter in the Universe (DM98), Santa Monica, California, Feb. 199