NUK - logo
E-viri
  • The I ceC ube prototype str...
    Ahrens, J.; Bai, X.; Barwick, S.W.; Bay, R.; Becker, J.K.; Boersma, D.J.; Böser, S.; Botner, O.; Bouchta, A.; Bouhali, O.; Braun, J.; Burgess, C.; Burgess, T.; Castermans, T.; Chinowsky, W.; Conrad, J.; Cooley, J.; Cowen, D.F.; Davour, A.; De Clercq, C.; DeYoung, T.; Desiati, P.; Ekström, P.; Feser, T.; Gaug, M.; Gaisser, T.K.; Ganugapati, R.; Gerhardt, L.; Goldschmidt, A.; Groß, A.; Hallgren, A.; Halzen, F.; Hanson, K.; Harenberg, T.; Helbing, K.; Hellwig, M.; Herquet, P.; Hubert, D.; Hughey, B.; Hulth, P.O.; Kampert, K.H.; Kelley, J.L.; Kohnen, G.; Köpke, L.; Kowalski, M.; Krasberg, M.; Leich, H.; Liubarsky, I.; Ludvig, J.; Lundberg, J.; Madsen, J.; Marciniewski, P.; Matis, H.S.; McParland, C.P.; Messarius, T.; Minaeva, Y.; Miočinović, P.; Morse, R.; Münich, K.S.; Nahnhauer, R.; Nam, J.; Neunhöffer, T.; Niessen, P.; Nygren, D.R.; Ögelman, H.; Olbrechts, Ph; Pérez de los Heros, C.; Pohl, A.C.; Porrata, R.; Price, P.B.; Rawlins, K.; Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Robbins, S.; Rodríguez Martino, J.; Schneider, D.; Schwarz, R.; Silvestri, A.; Solarz, M.; Sopher, J.; Spiczak, G.M.; Spiering, C.; Stamatikos, M.; Steffen, P.; Stokstad, R.G.; Sulanke, K.-H.; Taboada, I.; Thollander, L.; Tilav, S.; Wagner, W.; Walck, C.; Walter, M.; Wendt, C.; Wiebusch, C.H.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Yodh, G.

    Nuclear instruments & methods in physics research. Section A, Accelerators, spectrometers, detectors and associated equipment, 2006, Letnik: 556, Številka: 1
    Journal Article

    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.