by L. Bergström b for the AMANDA Collaboration:

• Main Authors: D. M. Lowder, T. Miller C, D. Nygren D, P. B. Price, A. Richards, S. W. Barwick, P. Mock, R. Porrata, E. Schneider, G. Yodh, E. C. Andrés, P. Askebjer, L. Bergström, A. Bouchta, E. Dahlberg, P. Ekström, B. Erl, A. Goobar, P. O. Hulth, Q. Sun, C. Walck, S. Carius, A. Hallgren, H. Rubinstein, K. Engel, L. Gray, F. Halzen, J. Jacobsen, I. Liubarsky, R. Morse, H. Heukenkamp, S. Hundertmark, A. Karle, Th. Mikolajski, T. Thon, C. Spiering
• Other Authors: The Pennsylvania State University CiteSeerX Archives
• Format: Text
• Language: English
• Published: 1996
• Subjects: South Pole; South pole
• Online Access: http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.255.4495; http://arxiv.org/pdf/astro-ph/9612122v1.pdf

At the AMANDA South Pole site, four new holes were drilled to depths 2050 m to 2180 m and instrumented with 86 photomultipliers (PMTs) at depths 1520-2000 m. Of these PMTs 79 are working, with 4-ns timing resolution and noise rates 300 to 600 Hz. Various diagnostic devices were deployed and are working. An observed factor 60 increase in scattering length and a sharpening of the distribution of arrival times of laser pulses relative to measurements at 800-1000 m showed that bubbles are absent below 1500 m. Absorption lengths are 100 to 150 m at wavelengths in the blue and UV to 337 nm. Muon coincidences are seen between the SPASE air shower array and the AMANDA PMTs at 800-1000 m and 1500-1900 m. The muon track rate is 30 Hz for 8-fold triggers and 10 Hz for 10-fold triggers. The present array is the nucleus for a future expanded array. The potential of AMANDA for SUSY dark matter search through the detection of high-energy neutrinos from the centre of the Sun or Earth is discussed. a