{"paper":{"title":"A Search for a Diffuse Flux of Astrophysical Muon Neutrinos with the IceCube 40-String Detector","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["hep-ex"],"primary_cat":"astro-ph.HE","authors_text":"A. Fedynitch, A. Franckowiak, A. Goldschmidt, A. Gro{\\ss}, A. Hallgren, A. Homeier, A. Ishihara, A. Kappes, A. Karle, A. Marotta, A. M. Brown, A. Olivas, A. O'Murchadha, A. Piegsa, A. R. Fazely, A. Rizzo, A. Sch\\\"onwald, A. Schukraft, A. Schultes, A. Silvestri, A. Slipak, A. St\\\"ossl, A. Tamburro, A. Tepe, A. Van Overloop, B. Christy, B. D. Fox, 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. Berley, D. Bertrand, D. Bindig, D. Bose, D. Chirkin, D. F. Cowen, D. Gora, D. Grant, D. Heinen, D. Hubert, D. J. Boersma, D. J. Koskinen, D. Pieloth, D. R. Nygren, D. Rutledge, D. R. Williams, D. Ryckbosch, D. Seckel, D. Tosi, D. Tur\\v{c}an, D. Z. Besson, E. A. Strahler, E. Bernardini, E. Blaufuss, 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. Stephens, G. T. Przybylski, G. W. Sullivan, G. Yodh, H.-G. Sander, H. Johansson, 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. Braun, J. C. Davis, J. C. D\\'iaz-V\\'elez, J. Clem, J. Daughhetee, J. Dreyer, J. Eisch, J. Gallagher, J.-H. K\\\"ohne, J. Jacobsen, J. J. Beatty, J. K. Becker, J. Kiryluk, J. L. Bazo Alba, J. L. Kelley, J. L\\\"unemann, J. Madsen, J. Miller, J. M. Joseph, J. P. Dumm, J. Petrovic, J.-P. H\\\"ul{\\ss}, J. Posselt, J. P. Rodrigues, 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. Schatto, K. Wiebe, K. Woschnagg, L. Demir\\\"ors, L. Gerhardt, L. Gladstone, L. K\\\"opke, L. Paul, M. Ahlers, M. Baker, M. Bissok, M. Carson, M. Danninger, M. Dierckxsens, M. Geisler, M. Gurtner, M. J. Larson, M. Kowalski, M. Krasberg, M. Labare, M. L. Benabderrahmane, M. Merck, M. M. Foerster, M. Olivo, M. Ono, M. Ribordy, M. Santander, M. Schunck, M. Stamatikos, M. St\\\"ur, M. V. D'Agostino, M. Vehring, M. Voge, M. Wallraff, M. Walter, M. Wolf, N. Milke, N. van Eijndhoven, N. Whitehorn, O. Botner, O. Depaepe, O. Engdeg{\\aa}rd, O. Fadiran, O. Schulz, P. A. Evenson, P. A. Toale, P. Berghaus, P. B. Price, P. Desiati, P. Herquet, P. Kenny, P. Majumdar, P. M\\'esz\\'aros, P. Nie{\\ss}en, P. O. Hulth, P. Redl, P. Roth, P. Zarzhitsky, Q. Swillens, R. Bay, R. Ehrlich, R. Franke, R. G. Stokstad, R. Lauer, R. Maruyama, R. Morse, R. Nahnhauer, R. Porrata, 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. Lafebre, S. M. Movit, S. Odrowski, S. Panknin, S. R. Klein, S. Sarkar, S. Seunarine, S. Stoyanov, S. Ter-Antonyan, S. Tilav, S. Toscano, S. W. Barwick, S. Westerhoff, S. Yoshida, T. Abu-Zayyad, T. Denger, T. DeYoung, T. Feusels, T. Fischer-Wasels, T. Gl\\\"usenkamp, T. Griesel, T. Karg, T. K. Gaisser, T. Kowarik, T. Krings, T. Kuwabara, T. Meures, T. Montaruli, T. Ruhe, T. R. Wood, T. Schmidt, T. Stanev, T. Stezelberger, T. Straszheim, T. Waldenmaier, U. Naumann, W. Huelsnitz, W. Rhode, X. Bai, X. W. Xu, Y. Abdou, Y. Sestayo","submitted_at":"2011-04-27T16:53:22Z","abstract_excerpt":"The IceCube Neutrino Observatory is a 1 km$^{3}$ detector currently taking data at the South Pole. One of the main strategies used to look for astrophysical neutrinos with IceCube is the search for a diffuse flux of high-energy neutrinos from unresolved sources. A hard energy spectrum of neutrinos from isotropically distributed astrophysical sources could manifest itself as a detectable signal that may be differentiated from the atmospheric neutrino background by spectral measurement. This analysis uses data from the IceCube detector collected in its half completed configuration which operated"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1104.5187","kind":"arxiv","version":5},"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"}