AMANDA is a high-energy neutrino telescope presently under construction at the geographical South Pole. In the Antarctic summer 1995/96, an array of 80 optical modules (OMs) arranged on 4 strings ...(AMANDA-B4) was deployed at depths between 1.5 and 2 km. In this paper we describe the design and performance of the AMANDA-B4 prototype, based on data collected between February and November 1996. Monte Carlo simulations of the detector response to down-going atmospheric muon tracks show that the global behavior of the detector is understood. We describe the data analysis method and present first results on atmospheric muon reconstruction and separation of neutrino candidates. The AMANDA array was upgraded with 216 OMs on 6 new strings in 1996/97 (AMANDA-B10), and 122 additional OMs on 3 strings in 1997/98.
The I ceC ube prototype string in A manda Ahrens, J.; Bai, X.; Barwick, S.W. ...
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
2006, Letnik:
556, Številka:
1
Journal Article
Recenzirano
The Antarctic Muon And Neutrino Detector Array (A
manda) is a high-energy neutrino telescope. It is a lattice of optical modules (OM) installed in the clear ice below the South Pole Station. Each OM ...contains a photomultiplier tube (PMT) that detects photons of Cherenkov light generated in the ice by muons and electrons. I
ceC
ube is a cubic-kilometer-sized expansion of A
manda currently being built at the South Pole. In I
ceC
ube the PMT signals are digitized already in the optical modules and transmitted to the surface. A prototype string of 41 OMs equipped with this new all-digital technology was deployed in the A
manda array in the year 2000. In this paper we describe the technology and demonstrate that this string serves as a proof of concept for the I
ceC
ube array. Our investigations show that the OM timing accuracy is 5
ns. Atmospheric muons are detected in excellent agreement with expectations with respect to both angular distribution and absolute rate.
IceCube is a large neutrino telescope of the next generation to be constructed in the Antarctic Ice Sheet near theSouth Pole. We present the conceptual design and the sensitivity of the IceCube ...detector to predicted fluxes of neutrinos, both atmospheric and extra-terrestrial. A complete simulation of the detector design has been used to study the detector's capability to search for neutrinos from sources such as active galaxies, and gamma-ray bursts.
New results from the AMANDA Neutrino Telescope Bernardini, Elisa; Ackermann, M.; Ahrens, J. ...
Nuclear physics. Section B, Proceedings supplement,
08/2005, Letnik:
145
Journal Article
The Antarctic Muon and Neutrino Detector Array (AMANDA) is a Čerenkov telescope which uses the south polar ice cap to search for neutrinos from extraterrestrial sources. We present a preliminary ...reconstruction of the energy spectrum of atmospheric neutrinos above a few TeV and several recent results on searches for high-energy astrophysical neutrinos, both non-localized and emitted by point-like sources.
We show new results from both the older and newer incarnations of AMANDA (AMANDA-B10 and AMANDA-II, respectively). These results demonstrate that AMANDA is a functioning, multipurpose detector with ...significant physics and astrophysics reach. They include a new higher-statistics measurement of the atmospheric muon neutrino flux and preliminary results from searches for a variety of sources of ultrahigh energy neutrinos: generic point sources, gamma-ray bursters and diffuse sources producing muons in the detector, and diffuse sources producing electromagnetic or hadronic showers in or near the detector.
We present new data taken with the AMANDA-II neutrino telescope array. The AMANDA-II upgrade was completed at the beginning of 2000. It significantly extends the sensitivity of the 10-string ...AMANDA-B10 detector to high- and ultrahigh-energy neutrino fluxes into regions of interest for probing current astrophysical models which remain unexplored by other experiments.
One vital means of raising energy efficiency is to introduce district heating in industry. The aim of this paper is to study factors which promote and inhibit district heating collaborations between ...industries and utilities. The human factors involved showed to affect district heating collaborations more than anything else does. Particularly
risk,
imperfect and asymmetric information,
credibility and trust,
inertia and
values are adequate variables when explaining the establishment or failure of industry-energy utility collaborations, while
heterogeneity,
access to capital and
hidden costs appear to be of lower importance. A key conclusion from this study is that in an industry-energy utility collaboration, it is essential to nurture the business relationship. In summary, successful collaboration depends more on the individuals and organizations involved in the relationship between the two parties than on the technology used in the collaboration.
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 ~ 10
4m
2, has been taking data since ...1997. Progress with calibration, investigation of ice properties, as well as muon and neutrino data analysis are described. The next stage 20-string detector AMANDA-II with ~ 800 PMTs will be completed in spring 2000.
We present the results of a search for point sources of high energy neutrinos in the northern hemisphere using AMANDA-II data collected in the year 2000. Included are flux limits on several AGN ...blazars, microquasars, magnetars and other candidate neutrino sources. A search for excesses above a random background of cosmic-ray-induced atmospheric neutrinos and misreconstructed downgoing cosmic-ray muons reveals no statistically significant neutrino point sources. We show that AMANDA-II has achieved the sensitivity required to probe known TeV gamma-ray sources such as the blazar Markarian 501 in its 1997 flaring state at a level where neutrino and gamma-ray fluxes are equal.
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