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@ARTICLE{Aartsen:319793,
author = {Aartsen, M. G. and Ackermann, M. and Adams, J. and Aguilar,
J. A. and Ahlers, M. and Ahrens, M. and Altmann, D. and
Andeen, K. and Anderson, T. and Ansseau, I. and Anton, G.
and Archinger, M. and Argüelles, C. and Auffenberg, J. and
Axani, S. and Bai, X. and Barwick, S. W. and Baum, V. and
Bay, R. and Beatty, J. J. and Becker Tjus, J. and Becker,
K.-H. and BenZvi, S. and Berley, D. and Bernardini, E. and
Bernhard, A. and Besson, D. Z. and Binder, G. and Bindig, D.
and Bissok, M. and Blaufuss, E. and Blot, S. and Bohm, C.
and Börner, M. and Bos, F. and Bose, D. and Böser, S. and
Botner, O. and Braun, J. and Brayeur, L. and Bretz, H.-P.
and Bron, S. and Burgman, A. and Carver, T. and Casier, M.
and Cheung, E. and Chirkin, D. and Christov, A. and Clark,
K. and Classen, L. and Coenders, S. and Collin, G. H. and
Conrad, J. M. and Cowen, D. F. and Cross, R. and Day, M. and
de André, J. P. A. M. and De Clercq, C. and del
Pino Rosendo, E. and Dembinski, H. and De Ridder, S. and
Desiati, P. and de Vries, K. D. and de Wasseige, G. and de
With, M. and DeYoung, T. and Díaz-Vélez, J. C. and di
Lorenzo, V. and Dujmovic, H. and Dumm, J. P. and Dunkman, M.
and Eberhardt, B. and Ehrhardt, T. and Eichmann, B. and
Eller, P. and Euler, S. and Evenson, P. A. and Fahey, S. and
Fazely, A. R. and Feintzeig, J. and Felde, J. and Filimonov,
K. and Finley, C. and Flis, S. and Fösig, C.-C. and
Franckowiak, A. and Friedman, E. and Fuchs, T. and Gaisser,
T. K. and Gallagher, J. and Gerhardt, L. and Ghorbani, K.
and Giang, W. and Gladstone, L. and Glauch, T. and
Gluesenkamp, Thorsten and Goldschmidt, A. and Gonzalez, J.
G. and Grant, D. and Griffith, Z. and Haack, C. and
Hallgren, A. and Halzen, F. and Hansen, E. and Hansmann, T.
and Hanson, K. and Hebecker, D. and Heereman, D. and
Helbing, K. and Hellauer, R. and Hickford, S. and Hignight,
J. and Hill, G. C. and Hoffman, K. D. and Hoffmann, R. and
Hoshina, K. and Huang, F. and Huber, M. and Hultqvist, K.
and In, S. and Ishihara, A. and Jacobi, E. and Japaridze, G.
S. and Jeong, M. and Jero, K. and Jones, B. J. P. and Kang,
W. and Kappes, Alexander and Karg, T. and Karle, A. and
Katz, U. and Kauer, M. and Keivani, A. and Kelley, J. L. and
Kheirandish, A. and Kim, J. and Kim, M. and Kintscher, T.
and Kiryluk, J. and Kittler, T. and Klein, S. R. and Kohnen,
G. and Koirala, R. and Kolanoski, H. and Konietz, R. and
Köpke, L. and Kopper, C. and Kopper, S. and Koskinen, D. J.
and Kowalski, M. and Krings, K. and Kroll, M. and Krückl,
G. and Krüger, C. and Kunnen, J. and Kunwar, S. and
Kurahashi, N. and Kuwabara, T. and Labare, M. and
Lanfranchi, J. L. and Larson, M. J. and Lauber, F. and
Lennarz, D. and Lesiak-Bzdak, M. and Leuermann, M. and Lu,
L. and Lünemann, J. and Madsen, J. and Maggi, G. and Mahn,
K. B. M. and Mancina, S. and Mandelartz, M. and Maruyama, R.
and Mase, K. and Maunu, R. and McNally, F. and Meagher, K.
and Medici, M. and Meier, M. and Meli, A. and Menne, T. and
Merino, G. and Meures, T. and Miarecki, S. and Montaruli, T.
and Moulai, M. and Nahnhauer, R. and Naumann, U. and Neer,
G. and Niederhausen, H. and Nowicki, S. C. and Nygren, D. R.
and Obertacke Pollmann, A. and Olivas, A. and
O’Murchadha, A. and Palczewski, T. and Pandya, H. and
Pankova, D. V. and Peiffer, P. and Penek, Ö. and Pepper, J.
A. and Pérez de los Heros, C. and Pieloth, D. and Pinat,
E. and Price, P. B. and Przybylski, G. T. and Quinnan, M.
and Raab, C. and Rädel, L. and Rameez, M. and Rawlins, K.
and Reimann, R. and Relethford, B. and Relich, M. and
Resconi, E. and Rhode, W. and Richman, M. and Riedel, B. and
Robertson, S. and Rongen, M. and Rott, C. and Ruhe, T. and
Ryckbosch, D. and Rysewyk, D. and Sabbatini, L. and
Sanchez Herrera, S. E. and Sandrock, A. and Sandroos, J.
and Sarkar, S. and Satalecka, K. and Schlunder, P. and
Schmidt, T. and Schoenen, S. and Schöneberg, S. and
Schumacher, L. and Seckel, D. and Seunarine, S. and Soldin,
D. and Song, M. and Spiczak, G. M. and Spiering, C. and
Stanev, T. and Stasik, A. and Stettner, J. and Steuer, A.
and Stezelberger, T. and Stokstad, R. G. and Stößl, A. and
Ström, R. and Strotjohann, N. L. and Sullivan, G. W. and
Sutherland, M. and Taavola, H. and Taboada, I. and Tatar, J.
and Tenholt, F. and Ter-Antonyan, S. and Terliuk, A. and
Tešić, G. and Tilav, S. and Toale, P. A. and Tobin, M. N.
and Toscano, S. and Tosi, D. and Tselengidou, M. and
Turcati, A. and Unger, E. and Usner, M. and Vandenbroucke,
J. and van Eijndhoven, N. and Vanheule, S. and van Rossem,
M. and van Santen, J. and Vehring, M. and Voge, M. and
Vogel, E. and Vraeghe, M. and Walck, C. and Wallace, A. and
Wallraff, M. and Wandkowsky, N. and Weaver, Ch. and Weiss,
M. J. and Wendt, C. and Westerhoff, S. and Whelan, B. J. and
Wickmann, S. and Wiebe, K. and Wiebusch, C. H. and Wille, L.
and Williams, D. R. and Wills, L. and Wolf, M. and Wood, T.
R. and Woolsey, E. and Woschnagg, K. and Xu, D. L. and Xu,
X. W. and Xu, Y. and Yanez, J. P. and Yodh, G. and Yoshida,
S. and Zoll, M.},
collaboration = {{IceCube Collaboration}},
title = {{S}earch for annihilating dark matter in the {S}un with
3 years of {I}ce{C}ube data},
journal = {The European physical journal / C},
volume = {77},
number = {3},
issn = {1434-6052},
address = {Berlin},
publisher = {Springer},
reportid = {PUBDB-2017-01471},
pages = {146},
year = {2017},
abstract = {We present results from an analysis looking for dark matter
annihilation in the Sun with the IceCube neutrino telescope.
Gravitationally trapped dark matter in the Sun’s core can
annihilate into Standard Model particles making the Sun a
source of GeV neutrinos. IceCube is able to detect neutrinos
with energies >100 GeV while its low-energy infill array
DeepCore extends this to >10 GeV. This analysis uses data
gathered in the austral winters between May 2011 and May
2014, corresponding to 532 days of livetime when the Sun,
being below the horizon, is a source of up-going neutrino
events, easiest to discriminate against the dominant
background of atmospheric muons. The sensitivity is a factor
of two to four better than previous searches due to
additional statistics and improved analysis methods
involving better background rejection and reconstructions.
The resultant upper limits on the spin-dependent dark
matter-proton scattering cross section reach down to
1.46×10$^{−5}$ pb for a dark matter particle of mass 500
GeV annihilating exclusively into
$\tau^{+}\tau^-$−particles. These are currently the most
stringent limits on the spin-dependent dark matter-proton
scattering cross section for WIMP masses above 50 GeV.},
cin = {ZEU-ICE},
ddc = {530},
cid = {I:(DE-H253)ZEU-ICE-20160806},
pnm = {613 - Matter and Radiation from the Universe (POF3-613)},
pid = {G:(DE-HGF)POF3-613},
experiment = {EXP:(DE-H253)IceCube-20150101},
typ = {PUB:(DE-HGF)16},
UT = {WOS:000400016600001},
doi = {10.1140/epjc/s10052-017-4689-9},
url = {https://bib-pubdb1.desy.de/record/319793},
}
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