Search for relativistic magnetic monopoles with the AMANDA-II neutrino telescope

• Published in: The European Physical Journal C
• Main Authors: Abbasi, R., Abdou, Y., Abu-Zayyad, T., Adams, J., Aguilar, J. A., Ahlers, M., Andeen, K., Auffenberg, J., Bai, X., Baker, Mark D., Barwick, S. W., Bay, R., Bazo Alba, J. L., Beattie, K., Beatty, J. J., Bechet, S., Becker, J. K., Becker, K.-H., Benabderrahmane, M. L., Benzvi, S., Berdermann, J., Berghaus, P., Berley, D., Bernardini, E., Bertrand, D., Besson, D. Z., Bissok, M., Blaufuss, E., Boersma, D. J., Bohm, C., Böser, S., Botner, O., Bradley, L., Braun, J., Buitink, S., Carson, M., Chirkin, D., Christy, B., Clem, J., Clevermann, F., Cohen, S., Colnard, C., Cowen, D. F., d'Agostino, M. V., Danninger, M., Davis, J. C., de Clercq, C., Demirörs, L., Depaepe, O., Descamps, F., Desiati, P., de Vries-Uiterweerd, G., Deyoung, T., Díaz-Vélez, J. C., Dierckxsens, M., Dreyer, J., Dumm, J. P., Duvoort, M. R., Ehrlich, R., Eisch, J., Ellsworth, R. W., Engdegård, O., Euler, S., Evenson, P. A., Fadiran, O., Fazely, A. R., Feusels, T., Filimonov, K., Finley, C., Foerster, M. M., Fox, B. D., Franckowiak, A., Franke, R., Gaisser, T. K., Gallagher, J., Geisler, M., Gerhardt, L., Gladstone, L., Glüsenkamp, T., Goldschmidt, A., Goodman, J. A., Grant, D., Griesel, T., Gross, A., Grullon, S., Gurtner, M., Ha, C., Hallgren, A., Halzen, F., Han, K., Hanson, K., Helbing, K., Herquet, P., Hickford, S., Hill, G. C., Hoffman, K. D., Homeier, A., Hoshina, K., Hubert, D., Huelsnitz, W., Hülss, J.-P., Hulth, P. O., Hultqvist, K., Hussain, S., Ishihara, A., Jacobsen, J., Japaridze, G. S., Johansson, H., Joseph, J. M., Kampert, K.-H., Karg, T., Karle, A., Kelley, J. L., Kemming, N., Kenny, P., Kiryluk, J., Kislat, F., Klein, S. R., Knops, S., Köhne, J.-H., Kohnen, G., Kolanoski, H., Köpke, L., Koskinen, D. J., Kowalski, M., Kowarik, T., Krasberg, M., Krings, T., Kroll, G., Kuehn, K., Kuwabara, T., Labare, M., Lafebre, S., Laihem, K., Landsman, H., Lauer, R., Lehmann, R., Lennarz, D., Lünemann, J., Madsen, Jens, Majumdar, P., Marotta, A., Maruyama, R., Mase, K., Matis, H. S., Matusik, M., Meagher, K., Merck, M., Mészáros, P., Meures, T., Middell, E., Milke, N., Miller, J., Montaruli, T., Morse, R., Movit, S. M., Nahnhauer, R., Nam, J. W., Naumann, U., Niessen, P., Nygren, D. R., Odrowski, S., Olivas, A., Olivo, M., O'Murchadha, A., Ono, M., Panknin, S., Paul, L., Pérez de Los Heros, C., Petrovic, J., Piegsa, A., Pieloth, D., Porrata, R., Posselt, J., Price, P. B., Prikockis, M., Przybylski, G. T., Rawlins, K., Redl, P., Resconi, E., Rhode, W., Ribordy, M., Rizzo, A., Rodrigues, J. P., Roth, P., Rothmaier, F., Rott, C., Roucelle, C., Ruhe, T., Rutledge, D., Ruzybayev, B., Ryckbosch, D., Sander, H.-G., Santander, M., Sarkar, S., Schatto, K., Schlenstedt, S., Schmidt, T., Schukraft, A., Schultes, A., Schulz, O., Schunck, M., Seckel, D., Semburg, B., Seo, S. H., Sestayo, Y., Seunarine, S., Silvestri, A., Slipak, A., Spiczak, G. M., Spiering, C., Stamatikos, M., Stanev, T., Stephens, G., Stezelberger, T., Stokstad, R. G., Stoyanov, S., Strahler, E. A., Straszheim, T., Sullivan, G. W., Swillens, Q., Taavola, H., Taboada, I., Tamburro, A., Tarasova, O., Tepe, A., Ter-Antonyan, S., Tilav, S., Toale, P. A., Toscano, S., Tosi, D., Turčan, D., van Eijndhoven, N., Vandenbroucke, J., van Overloop, A., van Santen, J., Voge, M., Voigt, B., Walck, C., Waldenmaier, T., Wallraff, M., Walter, M., Weaver, Ch., Wendt, C., Westerhoff, S., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wikström, G., Williams, D. R., Wischnewski, R., Wissing, H., Wolf, M., Woschnagg, K., Xu, C., Xu, X. W., Yodh, G., Yoshida, S., Zarzhitsky, P.
• Other Authors: APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Université Paris Sciences et Lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Sciences et Lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Université Paris Sciences et Lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Sciences et Lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
• Format: Article in Journal/Newspaper
• Language: English
• Published: CCSD 2010
• Subjects: [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]; [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]; [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]; [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]; Antarctic; The Antarctic; South Pole; Antarc*; Ice cap; South pole
• Online Access: https://in2p3.hal.science/in2p3-00706850; https://doi.org/10.1140/EPJC/S10052-010-1411-6

We present the search for Cherenkov signatures from relativistic magnetic monopoles in data taken with the AMANDA-II detector, a neutrino telescope deployed in the Antarctic ice cap at the Geographic South Pole. The non-observation of a monopole signal in data collected during the year 2000 improves present experimental limits on the flux of relativistic magnetic monopoles: Our flux limit varies between 3.8×10-17 cm-2 s-1 sr-1 (for monopoles moving at the vacuum speed of light) and 8.8×10-16 cm-2 s-1 sr-1 (for monopoles moving at a speed β= v/ c=0.76, just above the Cherenkov threshold in ice). These limits apply to monopoles that are energetic enough to penetrate the Earth and enter the detector from below the horizon. The limit obtained for monopoles reaching the detector from above the horizon is less stringent by roughly an order of magnitude, due to the much larger background from down-going atmospheric muons. This looser limit is however valid for a larger class of magnetic monopoles, since the monopoles are not required to pass through the Earth.