Search for Point Sources of High Energy Neutrinos with AMANDA

• Published in: The Astrophysical Journal
• Main Authors: Ahrens, J., Bai, X., Barouch, G., Barwick, S.W., Bay, R.C., Becka, T., Becker, K.H., Bertrand, D., Binon, F., Biron, A., Boeser, S., Botner, O., Bouchta, A., Bouhali, O., Burgess, T., Carius, S., Castermans, T., Chirkin, D., Conrad, J., Cooley, J., Cowen, D.F., Davour, A., Clercq, C.De, DeYoung, T., Desiati, P., Dewulf, J.P., Doksus, P., Edsjö, J., Ekström, P., Feser, T., Gaisser, T.K., Gaug, M., Gerhardt, L., Goldschmidt, A., Hallgren, A., Halzen, F., Hanson, K., Hardtke, R., Hauschildt, T., Hellwig, M., Herquet, P., Hill, G.C., Hulth, P.O., Hultqvist, K., Hundertmark, S., Jacobsen, J., Karle, A., Kim, J., Köpke, L., Kowalski, M., Kuehn, K., Lamoureux, J.I., Leich, H., Leuthold, M., Lindahl, P., Madsen, J., Marciniewski, P., Matis, H., McParland, C.P., Miller, T.C., Minaeva, Y., Miocinović, P., Mock, P.C., Morse, R., Neunhöffer, T., Niessen, P., Nygren, D.R., Ögelman, H., Olbrechts, P., los Heros, C.Pérez de, Pohl, A.C., Price, P.B., Przybylski, G.T., Rawlins, K., Resconi, E., Rhode, W., Ribordy, M., Richter, S., Martino, J.Rodríguez, Romenesko, P., Ross, D., Sander, H.G., Schmidt, T., Schneider, D., Schwarz, R., Silvestri, A., Solarz, M., Spiczak, G.M., Spiering, C., Steele, D., Steffen, P., Stokstad, R.G., Sulanke, K.H., Taboada, I., Thollander, L., Tilav, S., Walck, C., Weinheimer, C., Wiebusch, C.H., Wiedemann, C., Wischnewski, R., Wissing, H., Woschnagg, K., Wu, W., Yodh, G., Young, S.
• Language: English
• Published: 2002
• Subjects: Astrophysics and Astronomy; South Pole; South pole
• Online Access: https://doi.org/10.1086/345352; http://cds.cern.ch/record/574278

This paper describes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector, an array of 302 photomultiplier tubes, used for the detection of Cherenkov light from upward traveling neutrino-induced muons, buried deep in ice at the South Pole. The absolute pointing accuracy and angular resolution were studied by using coincident events between the AMANDA detector and two independent telescopes on the surface, the GASP air Cherenkov telescope and the SPASE extensive air shower array. Using data collected from April to October of 1997 (130.1 days of livetime), a general survey of the northern hemisphere revealed no statistically significant excess of events from any direction. The sensitivity for a flux of muon neutrinos is based on the effective detection area for through-going muons. Averaged over the Northern sky, the effective detection area exceeds 10,000 m^2 for E_{mu} ~ 10 TeV. Neutrinos generated in the atmosphere by cosmic ray interactions were used to verify the predicted performance of the detector. For a source with a differential energy spectrum proportional to E_{nu}^{-2} and declination larger than +40 degrees, we obtain E^2(dN_{nu}/dE) <= 10^{-6}GeVcm^{-2}s^{-1} for an energy threshold of 10 GeV. This paper describes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector, an array of 302 photomultiplier tubes, used for the detection of Cherenkov light from upward traveling neutrino-induced muons, buried deep in ice at the South Pole. The absolute pointing accuracy and angular resolution were studied by using coincident events between the AMANDA detector and two independent telescopes on the surface, the GASP air Cherenkov telescope and the SPASE extensive air shower array. Using data collected from April to October of 1997 (130.1 days of livetime), a general survey of the northern hemisphere revealed no statistically significant excess of events from any direction. The sensitivity for a flux of muon neutrinos is based on the effective detection area for through-going muons. Averaged over the Northern sky, the effective detection area exceeds 10,000 m^2 for E_{mu} ~ 10 TeV. Neutrinos generated in the atmosphere by cosmic ray interactions were used to verify the predicted performance of the detector. For a source with a differential energy spectrum proportional to E_{nu}^{-2} and declination larger than +40 degrees, we obtain E^2(dN_{nu}/dE) <= 10^{-6}GeVcm^{-2}s^{-1} for an energy threshold of 10 GeV.