Antarctic Muon and Neutrino Detector Array

March 24, 2000

  • We have completed the installation of six new strings during the 1999-2000 Antarctic summer season, completing the AMANDA-II array. You can see a schematic drawing of the array as it is now configured.
  • AMANDA in the news:
    • We are featured in Scientific American's new "Extreme Engineering" February 2000 issue, in the article "Seven Wonders of Modern Astronomy". Go here to see it.

Welcome to the AMANDA home page!

AMANDA is a detector being constructed at the South Pole, whose purpose is to observe high-energy (~ 1 TeV or 10^12 electron volt) neutrinos from astrophysical point sources. Strings of widely spaced photomultiplier tubes (PMTs) are placed into deep water-drilled holes in the South Polar ice cap. High energy neutrinos coming up through the earth will occasionally interact with ice or rock and create a muon; such a muon emits Cherenkov light when passing through the array, and it can be tracked by measuring the arrival times of these Cherenkov photons at the PMTs.

We successfully deployed 216 photomultiplier tubes (PMTs) and several diagnostic devices on 6 strings during the 1996-97 Antarctic summer season (Nov. 1996 - Feb. 1997). This completed the AMANDA-B detector, which consists of 302 PMTs on 10 strings at depths of 1500-2000 meters, and should have an effective detection area of approximately 10,000 m^2, based on Monte Carlo simulations. This detector has run for more than a year, and the 530 GBytes of data acquired during 1997 has now come back from the South Pole on tape. We are now in the process of analyzing this data. Go here or here for WWW-viewable technical papers.

During the 1997-98 season, we began the construction of AMANDA-II, which will have an effective area several times higher than AMANDA-B. Three strings were installed with modules that range from 1300 to 2400 meters in depth, and these will provide information on the optical properties of the polar ice over this large depth range and act as the first three strings of the new detector. We have completed AMANDA-II during the current Antarctic season (Nov. 1999 - Feb. 2000) with the addition of six new strings.

Who We Are
Here is the list of collaboration members.

Latest manuscripts
We have papers available with more detailed information on the current status of AMANDA and the status of the field of neutrino astronomy.

Detector Schematic
Here is a schematic view of the experiment showing locations of the strings.


Here are some events. This is real data, not Monte Carlo, and has just been updated with a very cool animated GIF of an event!

Gone Fishing
Here is a nontechnical (and very colorful and personal) history of AMANDA up to 1996 -- "Ice Fishing for Neutrinos" by Francis Halzen.

The AMANDA logo is available as a GIF picture or a gzipped Postscript file.

AMANDA Monte Carlo simulation software
RAVEN, the Monte Carlo package from the University of Wisconsin;
SIEGMUND, the code package maintained by DESY/Zeuthen.

AMANDA internal documents (private)
Here is the link to AMANDA internal documents; you must be a member of the collaboration and have the correct username and password to access this link.

Links to other places of interest:

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This page created by
Douglas M. Lowder
Department of Physics
University of California
Berkeley, CA 94720
Email: lowder@physics.berkeley.edu
WWW: http://amanda.berkeley.edu/lowder/