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| 2. |
- Miller, T. C., et al.
(författare)
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Particle astrophysics in antarctica
- 1996
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Ingår i: 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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Konferensbidrag (refereegranskat)
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| 3. |
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| 4. |
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| 5. |
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| 6. |
- Halzen, F., et al.
(författare)
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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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Ingår i: 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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Konferensbidrag (refereegranskat)
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| 7. |
- Mock, P. C., et al.
(författare)
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Status and capabilities of AMANDA-94
- 1995
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Ingår i: Proceedings, 24th International Conference, Rome, Italy, August 28-September 8, 1995.
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Konferensbidrag (refereegranskat)
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| 8. |
- Askebjer, P., et al.
(författare)
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On the age vs depth and optical clarity of deep ice at South Pole
- 1995
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Ingår i: Journal of Glaciology. - 0022-1430 .- 1727-5652. ; 41:139, s. 445-454
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Tidskriftsartikel (refereegranskat)abstract
- The first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800 to 1000 m in ice at the South Pole. During the 1995-96 season an additional six strings will be deployed at greater depths. Provided absorption, scattering, and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of \v{C}erenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth, and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the depth interval 1600 to 1800 m will be suitably transparent for the next six AMANDA strings and, moreover, that the interval 1600 to 2100 m will be suitably transparent for a future 1-km 3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 kyr BP.
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| 9. |
- Barwick, S. W., et al.
(författare)
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Initial results from the AMANDA high-energy neutrino detector
- 1998
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Ingår i: 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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Konferensbidrag (refereegranskat)
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| 10. |
- Bergstrom, L., et al.
(författare)
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The AMANDA experiment : Status and prospects for indirect dark matter detection
- 1996
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Ingår i: The identification of dark matter. Proceedings, 1st International Workshop, Sheffield, UK, September 8-12, 1996. ; , s. 521-528
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Konferensbidrag (refereegranskat)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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