| 1. |
- Halzen, F., et al.
(author)
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From the first neutrino telescope, the antarctic muon and neutrino detector array AMANDA, to the IceCube observatory
- 1999
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In: Proceedings of the 26th International Cosmic Ray Conference, August 17-25, 1999, Salt Lake City : Invited, Rapporteur, and Highlight Papers. - : American Institute of Physics (AIP). ; , s. 428-431
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Conference paper (peer-reviewed)
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| 2. |
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| 3. |
- Barwick, S. W., et al.
(author)
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Initial results from the AMANDA high-energy neutrino detector
- 1998
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In: High-energy physics. Proceedings, 29th International Conference, ICHEP'98, Vancouver, Canada, July 23-29, 1998. Vol. 1, 2. ; , s. 1447-1452
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Conference paper (peer-reviewed)
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| 4. |
- Miller, T. C., et al.
(author)
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Particle astrophysics in antarctica
- 1996
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In: International School of Cosmic Ray Astrophysics: 10th Course: Toward the Millennium in Astrophysics: Problems and Prospects 16-26 Jun 1996. Erice, Italy. ; , s. 157-166
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Conference paper (peer-reviewed)
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| 5. |
- Andres, EC, et al.
(author)
-
The AMANDA neutrino telescope
- 1999
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In: NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS. - : ELSEVIER SCIENCE BV. - 0920-5632. ; 77, s. 474-485
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Journal article (other academic/artistic)abstract
- With an effective telescope area of order 10(4) m(2) for TeV neutrinos, a threshold near similar to 50 GeV and a pointing accuracy of 2.5 degrees per muon track, the AMANDA detector represents the first of a new generation of high energy neutrino telescop
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| 6. |
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| 7. |
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| 8. |
- Wischnewski, R, et al.
(author)
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The AMANDA Neutrino Detector
- 1999
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In: NUCLEAR PHYSICS B-PROCEEDINGS SUPPLEMENTS. - : ELSEVIER SCIENCE BV. - 0920-5632. ; 75A, s. 412-414
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Journal article (other academic/artistic)abstract
- The first stage of the AMANDA High Energy Neutrino Detector at the South Pole, the 302 PMT array AMANDA-B with an expected effective area for TeV neutrinos of similar to 10(4) m(2), has been taking data since 1997. Progress with calibration, investigation
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| 9. |
- Bergstrom, L., et al.
(author)
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The AMANDA experiment : Status and prospects for indirect dark matter detection
- 1996
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In: The identification of dark matter. Proceedings, 1st International Workshop, Sheffield, UK, September 8-12, 1996. ; , s. 521-528
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Conference paper (peer-reviewed)abstract
- At the AMANDA South Pole site, four new holes were drilled to depths 2050m to 2180 m and instrumented with 86 photomultipliers (PMTs) at depths1520-2000 m. Of these PMTs 79 are working, with 4-ns timing resolutionand noise rates 300 to 600 Hz. Various diagnostic devices were deployedand are working. An observed factor 60 increase in scattering length anda sharpening of the distribution of arrival times of laser pulses relative tomeasurements 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 to337 nm. Muon coincidences are seen between the SPASE air shower arrayand the AMANDA PMTs at 800-1000 m and 1500-1900 m. The muon trackrate is 30 Hz for 8-fold triggers and 10 Hz for 10-fold triggers. The presentarray is the nucleus for a future expanded array. The potential of AMANDAfor SUSY dark matter search through the detection of high-energy neutrinosfrom the centre of the Sun or Earth is discussed.
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| 10. |
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| 11. |
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| 12. |
- Hulth, P. O., et al.
(author)
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The AMANDA experiment
- 1996
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In: Neutrino '96. Proceedings, 17th International Conference on Neutrino Physics and Astrophysics, Helsinki, Finland, June 13-19, 1996. ; , s. 518-523
-
Conference paper (peer-reviewed)abstract
- 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.
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| 13. |
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| 14. |
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| 15. |
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