{"paper":{"title":"Search for Galactic PeV Gamma Rays with the IceCube Neutrino Observatory","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. M. Brown, A. Obertacke, A. Olivas, A. O'Murchadha, A. R. Fazely, A. Sch\\\"onwald, A. Schukraft, A. Stasik, A. St\\\"o{\\ss}, A. Tamburro, A. Van Overloop, A. Zilles, B. Christy, B. Eberhardt, B. Riedel, B. Ruzybayev, C. Bohm, C. De Clercq, C. Finley, C. Ha, Ch. Weaver, C. H. Wiebusch, C. Kopper, C. P\\'erez de los Heros, C. Rott, C. Sheremata, C. Spiering, C. Walck, C. Wendt, C. Xu, D. Altmann, D. Berley, D. Bertrand, D. Bindig, D. Bose1, D. Chirkin, D. F. Cowen, D. G\\'ora, D. Grant, D. Heereman, D. Heinen, D. J. Boersma, D. J. Koskinen, D. L. Xu, D. Pieloth, D. R. Nygren, D. R. Williams, D. Ryckbosch, D. Seckel, D. Soldin, D. van der Drift, D. Z. Besson, E. A. Strahler, E. Bernardini, E. Blaufuss, E. Jacobi, E. Middell, E. Resconi, F. Clevermann, F. Descamps, F. Halzen, F. Kislat, F. McNally, F. Scheriau, G. C. Hill, G. de Vries-Uiterweerd, G. Golup, G. Kohnen, G. Kroll, G. M. Spiczak, G. S. Japaridze, G. T. Przybylski, G. W. Sullivan, G. Yodh, H.-G. Sander, H. Kolanoski, H. Landsman, H. S. Matis, H. Taavola, H. Wissing, IceCube Collaboration: M. G. Aartsen, I. Taboada, J. A. Aguilar, J. Adams, J. A. Goodman, J. A. Pepper, J. Auffenberg, J. Becker Tjus, J. Berdermann, J. Blumenthal, J. Brunner, J. Casey, J. C. Davis, J. C. D\\'iaz-V\\'elez, J. Daughhetee, J. Dreyer, J. Eisch, J. Feintzeig, J. Gallagher, J.-H. K\\\"ohne, J. Jacobsen, J. J. Beatty, J. Kiryluk, J. Kl\\\"as, J. Kunnen, J. L\\\"unemann, J. Madsen, J. Miller, J. P. Dumm, J. Posselt, J. P. Rodrigues, J. P. Yanez, J. van Santen, J. Ziemann, K. Andeen, K. Beattie, K. Clark, K. D. Hoffman, K. Filimonov, K. Frantzen, K. Hanson, K.-H. Becker, K. Helbing, K. Hoshina, K. Hultqvist, K. Mase, K. Meagher, K. Rawlins, K. Schatto, K. Wiebe, K. Woschnagg, L. Brayeur, L. Gerhardt, L. Gladstone, L. K\\\"opke, L. Mohrmann, L. Paul, L. R\\\"adel, L. Sch\\\"onherr, L. Schulte, M. Ackermann, M. Ahlers, M. Baker, M. Bell, M. Bissok, M. Carson, M. Casier, M. Danninger, M. Dunkman, M. Gurtner, M. J. Larson, M. Kowalski, M. Krasberg, M. Labare, M. L. Benabderrahmane, M. Lesiak-Bzdak, M. Merck, M. Olivo, M. Ribordy, M. Richman, M. Santander, M. Scheel, M. Schmitz, M. Soiron, M. Stamatikos, M. Usner, M. Vehring, M. Voge1, M. Vraeghe, M. Wallraff, M. Walter, M. W. E. Smith, M. Wolf, M. Zoll, N. Kurahashi, N. Milke, N. Pirk, N. van Eijndhoven, N. Whitehorn, O. Botner, O. Engdeg{\\aa}rd, O. Fadiran, O. Jlelati, O. Schulz, P. A. Evenson, P. A. Toale, P. Berghaus, P. B. Price, P. Desiati, P. Heimann, P. M\\'esz\\'aros, P. O. Hulth, P. Redl, P. Zarzhitsky, R. Abbasi, R. Bay, R. Bruijn, R. Eagan, R. Franke, R. G. Stokstad, R. Hellauer, R. Hoffmann, R. Lauer, R. Maruyama, R. Morse, R. Nahnhauer, R. Str\\\"om, R. Wasserman, R. W. Ellsworth, S. Bechet, S. BenZvi, S. Bohaichuk, S. B\\\"oser, S. Buitink, S. C. Nowicki, S. Cohen, S. De Ridder, S. Euler, S. Flis, S. Grullon, S. Hickford, S. H. Seo, S. Hussain, S. Kopper, S. Miarecki, S. M. Saba, S. Odrowski, S. Panknin, S. R. Klein, S. Sarkar, S. Schoenen, S. Sch\\\"oneberg, S. Seunarine, S. Ter-Antonyan, S. Tilav, S. Toscano, S. W. Barwick, S. Westerhoff, S. Yoshida, S. Zierke, T. DeYoung, T. Feusels, T. Fischer-Wasels, T. Fuchs, T. Gl\\\"usenkamp, T. Karg, T. K. Gaisser, T. Kuwabara, T. Meures, T. Montaruli, T. Ruhe, T. R. Wood, T. Salameh, 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":"2012-10-30T13:06:58Z","abstract_excerpt":"Gamma-ray induced air showers are notable for their lack of muons, compared to hadronic showers. Hence, air shower arrays with large underground muon detectors can select a sample greatly enriched in photon showers by rejecting showers containing muons. IceCube is sensitive to muons with energies above ~500 GeV at the surface, which provides an efficient veto system for hadronic air showers with energies above 1 PeV. One year of data from the 40-string IceCube configuration was used to perform a search for point sources and a Galactic diffuse signal. No sources were found, resulting in a 90% C"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1210.7992","kind":"arxiv","version":1},"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"}