Abstract
We present the results of the first IceCube search for dark matter annihilation in the center of the Earth. Weakly interacting massive particles (WIMPs), candidates for dark matter, can scatter off nuclei inside the Earth and fall below its escape velocity. Over time the captured WIMPs will be accumulated and may eventually self-annihilate. Among the annihilation products only neutrinos can escape from the center of the Earth. Large-scale neutrino telescopes, such as the cubic kilometer IceCube Neutrino Observatory located at the South Pole, can be used to search for such neutrino fluxes. Data from 327 days of detector livetime during 2011/2012 were analyzed. No excess beyond the expected background from atmospheric neutrinos was detected. The derived upper limits on the annihilation rate of WIMPs in the Earth and the resulting muon flux are an order of magnitude stronger than the limits of the last analysis performed with data from IceCube’s predecessor AMANDA. The limits can be translated in terms of a spin-independent WIMP–nucleon cross section. For a WIMP mass of 50 GeV this analysis results in the most restrictive limits achieved with IceCube data.
| Original language | English (US) |
|---|---|
| Article number | 82 |
| Journal | European Physical Journal C |
| Volume | 77 |
| Issue number | 2 |
| DOIs | |
| State | Published - Feb 1 2017 |
All Science Journal Classification (ASJC) codes
- Engineering (miscellaneous)
- Physics and Astronomy (miscellaneous)
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First search for dark matter annihilations in the Earth with the IceCube detector : IceCube Collaboration. / Aartsen, M. G.; Abraham, K.; Ackermann, M. et al.
In: European Physical Journal C, Vol. 77, No. 2, 82, 01.02.2017.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - First search for dark matter annihilations in the Earth with the IceCube detector
T2 - IceCube Collaboration
AU - Aartsen, M. G.
AU - Abraham, K.
AU - Ackermann, M.
AU - Adams, J.
AU - Aguilar, J. A.
AU - Ahlers, M.
AU - Ahrens, M.
AU - Altmann, D.
AU - Andeen, K.
AU - Anderson, T.
AU - Ansseau, I.
AU - Anton, G.
AU - Archinger, M.
AU - Argüelles, C.
AU - Auffenberg, J.
AU - Axani, S.
AU - Bai, X.
AU - Barwick, S. W.
AU - Baum, V.
AU - Bay, R.
AU - Beatty, J. J.
AU - Becker Tjus, J.
AU - Becker, K. H.
AU - BenZvi, S.
AU - Berley, D.
AU - Bernardini, E.
AU - Bernhard, A.
AU - Besson, D. Z.
AU - Binder, G.
AU - Bindig, D.
AU - Bissok, M.
AU - Blaufuss, E.
AU - Blot, S.
AU - Bohm, C.
AU - Börner, M.
AU - Bos, F.
AU - Bose, D.
AU - Böser, S.
AU - Botner, O.
AU - Braun, J.
AU - Brayeur, L.
AU - Bretz, H. P.
AU - Bron, S.
AU - Burgman, A.
AU - Carver, T.
AU - Casier, M.
AU - Cheung, E.
AU - Chirkin, D.
AU - Christov, A.
AU - Clark, K.
AU - Classen, L.
AU - Coenders, S.
AU - Collin, G. H.
AU - Conrad, J. M.
AU - Cowen, D. F.
AU - Cross, R.
AU - Day, M.
AU - de André, J. P.A.M.
AU - De Clercq, C.
AU - del Pino Rosendo, E.
AU - Dembinski, H.
AU - De Ridder, S.
AU - Desiati, P.
AU - de Vries, K. D.
AU - de Wasseige, G.
AU - de With, M.
AU - DeYoung, T.
AU - Díaz-Vélez, J. C.
AU - di Lorenzo, V.
AU - Dujmovic, H.
AU - Dumm, J. P.
AU - Dunkman, M.
AU - Eberhardt, B.
AU - Ehrhardt, T.
AU - Eichmann, B.
AU - Eller, P.
AU - Euler, S.
AU - Evenson, P. A.
AU - Fahey, S.
AU - Fazely, A. R.
AU - Feintzeig, J.
AU - Felde, J.
AU - Filimonov, K.
AU - Finley, C.
AU - Flis, S.
AU - Fösig, C. C.
AU - Franckowiak, A.
AU - Friedman, E.
AU - Fuchs, T.
AU - Gaisser, T. K.
AU - Gallagher, J.
AU - Gerhardt, L.
AU - Ghorbani, K.
AU - Giang, W.
AU - Gladstone, L.
AU - Glagla, M.
AU - Glauch, T.
AU - Glüsenkamp, T.
AU - Goldschmidt, A.
AU - Golup, G.
AU - Gonzalez, J. G.
AU - Grant, D.
AU - Griffith, Z.
AU - Haack, C.
AU - Haj Ismail, A.
AU - Hallgren, A.
AU - Halzen, F.
AU - Hansen, E.
AU - Hansmann, B.
AU - Hansmann, T.
AU - Hanson, K.
AU - Hebecker, D.
AU - Heereman, D.
AU - Helbing, K.
AU - Hellauer, R.
AU - Hickford, S.
AU - Hignight, J.
AU - Hill, G. C.
AU - Hoffman, K. D.
AU - Hoffmann, R.
AU - Holzapfel, K.
AU - Hoshina, K.
AU - Huang, F.
AU - Huber, M.
AU - Hultqvist, K.
AU - In, S.
AU - Ishihara, A.
AU - Jacobi, E.
AU - Japaridze, G. S.
AU - Jeong, M.
AU - Jero, K.
AU - Jones, B. J.P.
AU - Jurkovic, M.
AU - Kappes, A.
AU - Karg, T.
AU - Karle, A.
AU - Katz, U.
AU - Kauer, M.
AU - Keivani, A.
AU - Kelley, J. L.
AU - Kemp, J.
AU - Kheirandish, A.
AU - Kim, M.
AU - Kintscher, T.
AU - Kiryluk, J.
AU - Kittler, T.
AU - Klein, S. R.
AU - Kohnen, G.
AU - Koirala, R.
AU - Kolanoski, H.
AU - Konietz, R.
AU - Köpke, L.
AU - Kopper, C.
AU - Kopper, S.
AU - Koskinen, D. J.
AU - Kowalski, M.
AU - Krings, K.
AU - Kroll, M.
AU - Krückl, G.
AU - Krüger, C.
AU - Kunnen, J.
AU - Kunwar, S.
AU - Kurahashi, N.
AU - Kuwabara, T.
AU - Labare, M.
AU - Lanfranchi, J. L.
AU - Larson, M. J.
AU - Lauber, F.
AU - Lennarz, D.
AU - Lesiak-Bzdak, M.
AU - Leuermann, M.
AU - Leuner, J.
AU - Lu, L.
AU - Lünemann, J.
AU - Madsen, J.
AU - Maggi, G.
AU - Mahn, K. B.M.
AU - Mancina, S.
AU - Mandelartz, M.
AU - Maruyama, R.
AU - Mase, K.
AU - Maunu, R.
AU - McNally, F.
AU - Meagher, K.
AU - Medici, M.
AU - Meier, M.
AU - Meli, A.
AU - Menne, T.
AU - Merino, G.
AU - Meures, T.
AU - Miarecki, S.
AU - Mohrmann, L.
AU - Montaruli, T.
AU - Moulai, M.
AU - Nahnhauer, R.
AU - Naumann, U.
AU - Neer, G.
AU - Niederhausen, H.
AU - Nowicki, S. C.
AU - Nygren, D. R.
AU - Obertacke Pollmann, A.
AU - Olivas, A.
AU - O’Murchadha, A.
AU - Palczewski, T.
AU - Pandya, H.
AU - Pankova, D. V.
AU - Peiffer, P.
AU - Penek,
AU - Pepper, J. A.
AU - Pérez de los Heros, C.
AU - Pieloth, D.
AU - Pinat, E.
AU - Price, P. B.
AU - Przybylski, G. T.
AU - Quinnan, M.
AU - Raab, C.
AU - Rädel, L.
AU - Rameez, M.
AU - Rawlins, K.
AU - Reimann, R.
AU - Relethford, B.
AU - Relich, M.
AU - Resconi, E.
AU - Rhode, W.
AU - Richman, M.
AU - Riedel, B.
AU - Robertson, S.
AU - Rongen, M.
AU - Rott, C.
AU - Ruhe, T.
AU - Ryckbosch, D.
AU - Rysewyk, D.
AU - Sabbatini, L.
AU - Sanchez Herrera, S. E.
AU - Sandrock, A.
AU - Sandroos, J.
AU - Sarkar, S.
AU - Satalecka, K.
AU - Schimp, M.
AU - Schlunder, P.
AU - Schmidt, T.
AU - Schoenen, S.
AU - Schöneberg, S.
AU - Schumacher, L.
AU - Seckel, D.
AU - Seunarine, S.
AU - Soldin, D.
AU - Song, M.
AU - Spiczak, G. M.
AU - Spiering, C.
AU - Stahlberg, M.
AU - Stanev, T.
AU - Stasik, A.
AU - Stettner, J.
AU - Steuer, A.
AU - Stezelberger, T.
AU - Stokstad, R. G.
AU - Stößl, A.
AU - Ström, R.
AU - Strotjohann, N. L.
AU - Sullivan, G. W.
AU - Sutherland, M.
AU - Taavola, H.
AU - Taboada, I.
AU - Tatar, J.
AU - Tenholt, F.
AU - Ter-Antonyan, S.
AU - Terliuk, A.
AU - Tešić, G.
AU - Tilav, S.
AU - Toale, P. A.
AU - Tobin, M. N.
AU - Toscano, S.
AU - Tosi, D.
AU - Tselengidou, M.
AU - Turcati, A.
AU - Unger, E.
AU - Usner, M.
AU - Vandenbroucke, J.
AU - van Eijndhoven, N.
AU - Vanheule, S.
AU - van Rossem, M.
AU - van Santen, J.
AU - Veenkamp, J.
AU - Vehring, M.
AU - Voge, M.
AU - Vogel, E.
AU - Vraeghe, M.
AU - Walck, C.
AU - Wallace, A.
AU - Wallraff, M.
AU - Wandkowsky, N.
AU - Weaver, Ch
AU - Weiss, M. J.
AU - Wendt, C.
AU - Westerhoff, S.
AU - Whelan, B. J.
AU - Wickmann, S.
AU - Wiebe, K.
AU - Wiebusch, C. H.
AU - Wille, L.
AU - Williams, D. R.
AU - Wills, L.
AU - Wolf, M.
AU - Wood, T. R.
AU - Woolsey, E.
AU - Woschnagg, K.
AU - Xu, D. L.
AU - Xu, X. W.
AU - Xu, Y.
AU - Yanez, J. P.
AU - Yodh, G.
AU - Yoshida, S.
AU - Zoll, M.
N1 - Funding Information: We acknowledge the support from the following agencies: U.S. National Science Foundation-Office of Polar Programs, U.S. National Science Foundation-Physics Division, University of Wisconsin Alumni Research Foundation, the Grid Laboratory Of Wisconsin (GLOW) grid infrastructure at the University of Wisconsin-Madison, the Open Science Grid (OSG) grid infrastructure; U.S. Department of Energy, and National Energy Research Scientific Computing Center, the Louisiana Optical Network Initiative (LONI) grid computing resources; Natural Sciences and Engineering Research Council of Canada, WestGrid and Compute/Calcul Canada; Swedish Research Council, Swedish Polar Research Secretariat, Swedish National Infrastructure for Computing (SNIC), and Knut and Alice Wallenberg Foundation, Sweden; German Ministry for Education and Research (BMBF), Deutsche Forschungsgemeinschaft (DFG), Helmholtz Alliance for Astroparticle Physics (HAP), Research Department of Plasmas with Complex Interactions (Bochum), Germany; Fund for Scientific Research (FNRS-FWO), FWO Odysseus programme, Flanders Institute to encourage scientific and technological research in industry (IWT), Belgian Federal Science Policy Office (Belspo); University of Oxford, United Kingdom; Marsden Fund, New Zealand; Australian Research Council; Japan Society for Promotion of Science (JSPS); the Swiss National Science Foundation (SNSF), Switzerland; National Research Foundation of Korea (NRF); Villum Fonden, Danish National Research Foundation (DNRF), Denmark. Publisher Copyright: © 2017, The Author(s).
PY - 2017/2/1
Y1 - 2017/2/1
N2 - We present the results of the first IceCube search for dark matter annihilation in the center of the Earth. Weakly interacting massive particles (WIMPs), candidates for dark matter, can scatter off nuclei inside the Earth and fall below its escape velocity. Over time the captured WIMPs will be accumulated and may eventually self-annihilate. Among the annihilation products only neutrinos can escape from the center of the Earth. Large-scale neutrino telescopes, such as the cubic kilometer IceCube Neutrino Observatory located at the South Pole, can be used to search for such neutrino fluxes. Data from 327 days of detector livetime during 2011/2012 were analyzed. No excess beyond the expected background from atmospheric neutrinos was detected. The derived upper limits on the annihilation rate of WIMPs in the Earth and the resulting muon flux are an order of magnitude stronger than the limits of the last analysis performed with data from IceCube’s predecessor AMANDA. The limits can be translated in terms of a spin-independent WIMP–nucleon cross section. For a WIMP mass of 50 GeV this analysis results in the most restrictive limits achieved with IceCube data.
AB - We present the results of the first IceCube search for dark matter annihilation in the center of the Earth. Weakly interacting massive particles (WIMPs), candidates for dark matter, can scatter off nuclei inside the Earth and fall below its escape velocity. Over time the captured WIMPs will be accumulated and may eventually self-annihilate. Among the annihilation products only neutrinos can escape from the center of the Earth. Large-scale neutrino telescopes, such as the cubic kilometer IceCube Neutrino Observatory located at the South Pole, can be used to search for such neutrino fluxes. Data from 327 days of detector livetime during 2011/2012 were analyzed. No excess beyond the expected background from atmospheric neutrinos was detected. The derived upper limits on the annihilation rate of WIMPs in the Earth and the resulting muon flux are an order of magnitude stronger than the limits of the last analysis performed with data from IceCube’s predecessor AMANDA. The limits can be translated in terms of a spin-independent WIMP–nucleon cross section. For a WIMP mass of 50 GeV this analysis results in the most restrictive limits achieved with IceCube data.
UR - http://www.scopus.com/inward/record.url?scp=85012226063&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85012226063&partnerID=8YFLogxK
U2 - 10.1140/epjc/s10052-016-4582-y
DO - 10.1140/epjc/s10052-016-4582-y
M3 - Article
AN - SCOPUS:85012226063
VL - 77
JO - European Physical Journal C
JF - European Physical Journal C
SN - 1434-6044
IS - 2
M1 - 82
ER -