| Summary: | INTRODUCTION AND SUMMARY The Antarctic Muon and Neutrino Detector Array AMANDA is a multi-purpose instrument; its science missions cover particle physics, astronomy and astrophysics, cosmology and cosmic ray physics[1]. Its deployment creates new opportunities for glaciology[2]. The first-generation detector is designed to reach a relatively large telescope area and detection volume for a neutrino threshold not higher than 100 GeV. This relatively low threshold permits calibration of the novel instrument on the known flux of atmospheric neutrinos. Its architecture has been optimized for reconstructing the Cherenkov light front radiated by up-going, neutrino-induced muons which must be identified in a background of down-going, cosmic ray muons which are more than 10 5 times more frequent for a depth of 1--2 kilometer. The status of the AMANDA project can be summarized as follows: ffl Construction of the first generation AMANDA detector[3] was
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