NEXT 100 is a neutrinoless double beta decay search experiment scheduled for installation at the Laboratorio Subterrneo de Canfranc (LSC) in 2013. The NEXT 100 detector is a Time Projection Chamber ...(TPC) utilizing the default technology solution of a electroluminescence signal amplification. NEXT 1 EL is an important milestone in the development of NEXT 100 which aims to demonstrate large size EL amplification and long track drift in 10 bar pressure Xe gas.
The paper evaluates the effectiveness of the electromechanical shock absorber for a subway car based on dynamic quality indicators. To determine them, a method of synthesis
of random forced vertical ...oscillations of a dynamic model of a subway car was developed,
which is based on the method of sliding summation taking into account the spectral density
obtained when processing the test results of a subway car. Also in the work the technique on
definition of indicators of dynamic quality of the metrocar with electromechanical shockabsorbers which is based on modeling of processes of movement of the subway car on a site
of a way with casual roughness and definition, by results of modeling, indicators of dynamic
quality is created. The study of forced random oscillations of the dynamic model of a
subway car showed that the spring suspension based on electromechanical shock absorbers
has a significant advantage over the central spring suspension for all quality indicators in
the entire range of speeds. The dependence of the average power generated by the shock
absorber is established.
Muon track reconstruction and data selection techniques in AMANDA Ahrens, J.; Bai, X.; Bay, R. ...
Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment,
05/2004, Letnik:
524, Številka:
1
Journal Article
Recenzirano
Odprti dostop
The Antarctic Muon And Neutrino Detector
Array (AMANDA) is a high-energy neutrino telescope operating at the geographic South Pole. It is a lattice of photo-multiplier tubes buried deep in the polar ...ice between 1500 and
2000
m
. The primary goal of this detector is to discover astrophysical sources of high-energy neutrinos. A high-energy muon neutrino coming through the earth from the Northern Hemisphere can be identified by the secondary muon moving upward through the detector.
The muon tracks are reconstructed with a maximum likelihood method. It models the arrival times and amplitudes of Cherenkov photons registered by the photo-multipliers. This paper describes the different methods of reconstruction, which have been successfully implemented within
AMANDA. Strategies for optimizing the reconstruction performance and rejecting background are presented. For a typical analysis procedure the direction of tracks are reconstructed with about 2° accuracy.
Neutrinos are elementary particles that carry no electric charge and have little mass. As they interact only weakly with other particles, they can penetrate enormous amounts of matter, and therefore ...have the potential to directly convey astrophysical information from the edge of the Universe and from deep inside the most cataclysmic high-energy regions. The neutrino's great penetrating power, however, also makes this particle difficult to detect. Underground detectors have observed low-energy neutrinos from the Sun and a nearby supernova, as well as neutrinos generated in the Earth's atmosphere. But the very low fluxes of high-energy neutrinos from cosmic sources can be observed only by much larger, expandable detectors in, for example, deep water or ice. Here we report the detection of upwardly propagating atmospheric neutrinos by the ice-based Antarctic muon and neutrino detector array (AMANDA). These results establish a technology with which to build a kilometre-scale neutrino observatory necessary for astrophysical observations.
Thesis (Ph. D.)--University of Wisconsin--Madison, 1997.
Typescript. eContent provider-neutral record in process. Description based on print version record. Includes bibliographical references ...(leaves 159-163).
To date, Antarctic Muon and Neutrino Detector Array (AMANDA) collaboration has successfully deployed 382 optical modules at various depths in the South Polar ice sheet. The last 216 optical modules ...were put in place during the 1996-7 austral summer. This deployment completed a 10-stringed detector at depth between 1500-2000m (AMANDA-B). The detector has been operating successfully and taking data at a rate of $92Hz$. However, due to the remoteness of location and the limited bandwidth for satellite transmission, only 5% of the latest data can be transmitted from the South Pole to the collaboration. Before the end of the 1996-7 antarctic season 6$GBytes$ of data were carried to the rest of the world by hand. Since this data was taken while detector calibration was still being performed, it is far from ideal. Yet this sample, to date, represents the largest amount of the data taken by the 10 string detector available for analysis. A total of 11.8 hours of raw data was analysed, comprising 3,380,739 events. Of that number 2,951,118 were AMANDA-B triggers. After calibration and noise cleaning, the number of confirmed AMANDA-B triggers was further reduced to 2,880,391. From this data set a fraction of events were reconstructed without any filtering on the reconstructed direction of the final track. This resulted in 103,168 reconstructed tracks from all zenith angles. However, the full set of 2,880,391 triggers was used to reconstruct tracks, selecting only those that yielded an up-going muon. The procedure produced 25,122 tracks. Various quality criteria was then utilised to discriminate real up-going tracks from fake events mimicked by down-going muons. No real up-going events were found. My personal contribution to the AMANDA experiment has been in three main areas: hardware; I have built 40 of the first AMANDA-A modules; software; I have written subroutines for the University of Wisconsin-Madison AMANDA group's Monte Carlo; data analysis; I have analysed the early 10 string AMANDA-B data.
PDF
