The AMANDA collaboration has successfully deployed a 10-string array (AMANDA-B10) of 302 photomultiplier tubes at the South Pole at a depth of 1.5 to 1.9 km. The array has been used to measure the optical quality of the ice, reconstruct tracks from high-energy cosmic ray muons, and measure the energy of electromagnetic cascades. Simulations and early analyses of data indicate that the array has an effective area of ~ 10,000 m(2) for throughgoing neutrino-induced muons, with an angular resolution of 2.5(deg) and good rejection (> 10(5) ) of down-going cosmic ray muons. I will describe the design and construction of the detector, the methods used to simulate its performance and to reconstruct muon tracks, and the results to date; I will include a progress report on the ongoing analysis of a full year of data (500 GB) from the detector. Finally, I will discuss future work; this will include a description of the AMANDA-II array, already begun with three strings in 1997-98, which will have an effective area of up to ~ 10(5) m(2) and angular resolution of ~ 1(deg) .
American Astronomical Society Meeting Abstracts #192
- Pub Date:
- May 1998