{"paper":{"title":"IceCube Sensitivity for Low-Energy Neutrinos from Nearby Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Fedynitch, A. Franckowiak, A. Goldschmidt, A. Gro{\\ss}, A. Haj Ismail, A. Hallgren, A. H. Cruz Silva, A. Homeier, A. Ishihara, A. Kappes, A. Karle, A. Marotta, A. M. Brown, A. Olivas, A. O'Murchadha, A. Piegsa, A. R. Fazely, A. Sch\\\"onwald, A. Schukraft, A. Schultes, A. Silvestri, A. Slipak, A. S. Richard, A. St\\\"o{\\ss}l, A. Tamburro, A. Tepe, A. Van Overloop, B. Christy, B. D. Fox, B. Hoffmann, B. Ruzybayev, B. Semburg, C. Bohm, C. Colnard, C. De Clercq, C. Finley, C. Ha, Ch. Weaver, C. H. Wiebusch, C. P\\'erez de los Heros, C. Rott, C. Spiering, C. Walck, C. Wendt, C. Xu, D. Altmann, D. Berley, D. Bertrand, D. Bindig, D. Bose, D. Chirkin, D. F. Cowen, D. G\\'ora, D. Grant, D. Heinen, D. J. Boersma, D. J. Koskinen, D. L. Xu, D. Pieloth, D. R. Nygren, D. Rutledge, D. R. Williams, D. Ryckbosch, D. Seckel, D. Tosi, D. Z. Besson, E. A. Strahler, E. Bernardini, E. Blaufuss, E. Jakobi, E. Middell, E. Resconi, F. Clevermann, F. Descamps, F. Halzen, F. Kislat, F. Rothmaier, G. C. Hill, G. de Vries-Uiterweerd, G. Kohnen, G. Kroll, G. M. Spiczak, G. S. Japaridze, G. T. Przybylski, G. W. Sullivan, G. Yodh, H.-G. Sander, H. Johansson, H. K\\\"ohne, H. Kolanoski, H. Landsman, H. S. Matis, H. Taavola, H. Wissing, IceCube Collaboration: R. Abbasi, I. Taboada, J. A. Aguilar, J. Adams, J. A. Goodman, J. Auffenberg, J. Berdermann, J. Blumenthal, J. C. Davis, J. C. Diaz-V\\'elez, J. Daughhetee, J. Dreyer, J. Eisch, J. Feintzeig, J. Gallagher, J. Jacobsen, J. J. Beatty, J. K. Becker, J. Kiryluk, J. L. Bazo Alba, J. L\\\"unemann, J. Madsen, J. Miller, J. P. Dumm, J. Petrovic, J.-P. H\\\"ul{\\ss}, J. Posselt, J. P. Rodrigues, J. P. Yanez, J. Vandenbroucke, J. van Santen, J. W. Nam, K. Andeen, K. Beattie, K. D. Hoffman, K. Filimonov, K. Han, K. Hanson, K.-H. Becker, K. Helbing, K.-H. Kampert, K. Hoshina, K. Hultqvist, K. Laihem, K. Mase, K. Meagher, K. Rawlins, K. S. Caballero-Mora, K. Schatto, K. Singh, K. Wiebe, K. Woschnagg, L. Demir\\\"ors, L. Gerhardt, L. Gladstone, L. K\\\"opke, L. Paul, L. Schulte, M. Ackermann, M. Ahlers, M. Baker, M. Bissok, M. Carson, M. Danninger, M. Dierckxsens, M. Dunkman, M. Gurtner, M. J. Larson, M. Kowalski, M. Krasberg, M. Labare, M. L. Benabderrahmane, M. M. Allen, M. Merck, M. Olivo, M. Ribordy, M. Richman, M. Santander, M. Schunck, M. Stamatikos, M. St\\\"uer, M. V. D'Agostino, M. Vehring, M. Voge, M. Wallraff, M. Walter, M. Wolf, M. Zoll, N. Kurahashi, N. Milke, N. van Eijndhoven, N. Whitehorn, O. Botner, O. Engdeg{\\aa}rd, O. Fadiran, O. Schulz, P. A. Evenson, P. A. Toale, P. Berghaus, P. B. Price, P. Desiati, P. Kenny, P. M\\'esz\\'aros, P. O. Hulth, P. Redl, P. Zarzhitsky, Q. Swillens, R. Bay, R. Franke, R. G. Stokstad, R. Hellauer, R. Lauer, R. Maruyama, R. Morse, R. Nahnhauer, R. Porrata, R. Str\\\"om, R. W. Ellsworth, R. Wischnewski, S. Bechet, S. BenZvi, S. B\\\"oser, S. Buitink, S. Cohen, S. Euler, S. Grullon, S. Hickford, S. H. Seo, S. Hussain, S. Kopper, S. Miarecki, S. M. Movit, S. Odrowski, S. Panknin, S. R. Klein, S. Sarkar, S. Seunarine, S. Ter-Antonyan, S. Tilav, S. Toscano, S. W. Barwick, S. Westerhoff, S. Yoshida, T. Abu-Zayyad, T. Degner, T. DeYoung, T. Feusels, T. Fischer-Wasels, T. Gl\\\"usenkamp, T. Griesel, T. Karg, T. K. Gaisser, T. Kowarik, T. Kuwabara, T. Meures, T. Montaruli, T. Ruhe, T. R. Wood, T. Schmidt, T. Stanev, T. Stezelberger, T. Waldenmaier, U. Naumann, V. Baum, W. Huelsnitz, W. Rhode, X. Bai, X. W. Xu, Y. Abdou, Y. Sestayo","submitted_at":"2011-07-31T12:51:41Z","abstract_excerpt":"This paper describes the response of the IceCube neutrino telescope located at the geographic South Pole to outbursts of MeV neutrinos from the core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a volume of ~ 1 cubic kilometer in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect large numbers of M"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1108.0171","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}