Searches for Connections between Dark Matter and High-Energy Neutrinos with IceCube
Creators: name: Abbasi, R.
name: Ackermann, M.
name: Adams, J.
name: Aguilar, J. A.
name: Ahlers, M.
name: Ahrens, M.
name: Alameddine, J. M.
name: Alves, Jr. A. A.
name: Amin, N. M.
name: Andeen, K.
name: Anderson, T.
name: Anton, G.
name: Argüelles, C.
name: Ashida, Y.
name: Athanasiadou, Sofia
name: Axani, S.
name: Bai, X.
name: Balagopal, V. A.
name: Baricevic, M.
name: Barwick, S. W.
name: Basu, V.
name: Baur, S.
name: Bay, R.
name: Beatty, J. J.
name: Becker, K.-H.
name: Becker Tjus, J.
name: Beise, J.
name: Bellenghi, C.
name: Benda, S.
name: BenZvi, S.
name: Berley, D.
name: Bernardini, E.
name: Besson, D. Z.
name: Binder, G.
name: Bindig, D.
name: Blaufuss, E.
name: Blot, Summer
name: Bontempo, F.
name: Book, J. Y.
name: Borowka, J.
name: Böser, S.
name: Botner, O.
name: Böttcher, J.
name: Bourbeau, E.
name: Bradascio, Federica
name: Braun, J.
name: Brinson, B.
name: Bron, S.
name: Brostean-Kaiser, Jannes
name: Burley, R. T.
name: Busse, R. S.
name: Campana, M. A.
name: Carnie-Bronca, E. G.
name: Chen, C.
name: Chen, Z.
name: Chirkin, D.
name: Choi, K.
name: Clark, B. A.
name: Clark, K.
name: Classen, L.
name: Coleman, A.
name: Collin, G. H.
name: Connolly, A.
name: Conrad, J. M.
name: Coppin, P.
name: Correa, P.
name: Cowen, D. F.
name: Cross, R.
name: Dappen, C.
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name: López, D. Delgado
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name: de Vries, K. D.
name: de Wasseige, G.
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name: Dittmer, M.
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name: Erpenbeck, H.
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name: Evenson, P. A.
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name: Fienberg, A. T.
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name: Klein, S. R.
name: Kochocki, A.
name: Koirala, R.
name: Kolanoski, H.
name: Kontrimas, T.
name: Köpke, L.
name: Kopper, C.
name: Kopper, S.
name: Koskinen, D. J.
name: Koundal, P.
name: Kovacevich, M.
name: Kowalski, Marek
name: Kozynets, T.
name: Krupczak, E.
name: Kun, E.
name: Kurahashi, N.
name: Lad, Neha Navnitkumar
name: Gualda, C. Lagunas
name: Larson, M. J.
name: Lauber, F.
name: Lazar, J. P.
name: Lee, J. W.
name: Leonard, K.
name: Leszczyńska, A.
name: Lincetto, M.
name: Liu, Q. R.
name: Liubarska, M.
name: Lohfink, E.
name: Mariscal, C. J. Lozano
name: Lu, L.
name: Lucarelli, F.
name: Ludwig, A.
name: Luszczak, W.
name: Lyu, Y.
name: Ma, Wing Yan
name: Madsen, J.
name: Mahn, K. B. M.
name: Makino, Y.
name: Mancina, S.
name: Sainte, W. Marie
name: Mariş, I. C.
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name: Maruyama, R.
name: McCarthy, S.
name: McElroy, T.
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name: Mead, J. V.
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name: Moore, R. W.
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name: Mukherjee, T.
name: Naab, Richard
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name: Naumann, U.
name: Necker, Jannis David
name: Nguyễn, L. V.
name: Niederhausen, H.
name: Nisa, M. U.
name: Nowicki, S. C.
name: Pollmann, A. Obertacke
name: Oehler, M.
name: Oeyen, B.
name: Olivas, A.
name: Osborn, J.
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name: Park, N.
name: Parker, G. K.
name: Paudel, E. N.
name: Paul, L.
name: de los Heros, C. Pérez
name: Peters, L.
name: Peterson, J.
name: Philippen, S.
name: Pieper, S.
name: Pizzuto, A.
name: Plum, M.
name: Popovych, Y.
name: Porcelli, A.
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name: Pries, B.
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name: Reusch, Simeon
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name: Richman, M.
name: Riedel, B.
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name: Robertson, S.
name: Roellinghoff, G.
name: Rongen, M.
name: Rott, C.
name: Ruhe, T.
name: Ryckbosch, D.
name: Cantu, D. Rysewyk
name: Safa, I.
name: Saffer, J.
name: Salazar-Gallegos, D.
name: Sampathkumar, P.
name: Herrera, S. E. Sanchez
name: Sandrock, A.
name: Santander, M.
name: Sarkar, S.
name: Sarkar, S.
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name: Schneider, A.
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name: Shefali, S.
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name: Skrzypek, B.
name: Smithers, B.
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name: Sogaard, A.
name: Soldin, D.
name: Spannfellner, C.
name: Spiczak, G. M.
name: Spiering, C.
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name: Stanev, T.
name: Stein, Robert
name: Stettner, J.
name: Stezelberger, T.
name: Stürwald, T.
name: Stuttard, T.
name: Sullivan, G. W.
name: Taboada, I.
name: Ter-Antonyan, S.
name: Thwaites, J.
name: Tilav, S.
name: Tollefson, K.
name: Tönnis, C.
name: Toscano, S.
name: Tosi, D.
name: Trettin, Alexander
name: Tselengidou, M.
name: Tung, C. F.
name: Turcati, A.
name: Turcotte, R.
name: Twagirayezu, J. P.
name: Ty, B.
name: Unland Elorrieta, M. A.
name: Upshaw, K.
name: Valtonen-Mattila, N.
name: Vandenbroucke, J.
name: van Eijndhoven, N.
name: Vannerom, D.
name: Santen, Jakob van
name: Veitch-Michaelis, J.
name: Verpoest, S.
name: Walck, C.
name: Wang, W.
name: Watson, T. B.
name: Weaver, C.
name: Weigel, P.
name: Weindl, A.
name: Weldert, J.
name: Wendt, C.
name: Werthebach, J.
name: Weyrauch, M.
name: Whitehorn, N.
name: Wiebusch, C. H.
name: Willey, N.
name: Williams, D. R.
name: Wolf, M.
name: Wrede, G.
name: Wulff, J.
name: Xu, X. W.
name: Yanez, J. P.
name: Yildizci, E.
name: Yoshida, S.
name: Yu, S.
name: Yuan, T.
name: Zhang, Z.
name: IceCube Collaboration
Publisher: name: Deutsches Elektronen-Synchrotron, DESY, Hamburg
Year: 2022
Subjects: dark matter: leptonic decay
muon: pair production
bottom: pair production
dark matter: annihilation
neutrino: cosmic radiation
galaxy: dark matter
dark matter: signature
dark matter: scalar
fermion: dark matter
dark matter: lifetime
neutrino: interaction
dark matter: mass
dark matter: decay
cross section: annihilation
neutrino: scattering
mediation
IceCube
anisotropy
coupling constant: upper limit
experimental results

description: In this work, we present the results of searches for signatures of dark matter decay or annihilation into Standard Model particles, and secret neutrino interactions with dark matter. Neutrinos could be produced in the decay or annihilation of galactic or extragalactic dark matter. Additionally, if an interaction between dark matter and neutrinos exists then dark matter will interact with extragalactic neutrinos. In particular galactic dark matter will induce an anisotropy in the neutrino sky if this interaction is present. We use seven and a half years of the High-Energy Starting Event (HESE) sample data, which measures neutrinos in the energy range of approximately 60 TeV to 10 PeV, to study these phenomena. This all-sky event selection is dominated by extragalactic neutrinos. For dark matter of $\sim$ 1 PeV in mass, we constrain the velocity-averaged annihilation cross section to be smaller than $10^{-23}$cm$^3$/s for the exclusive $\mu^+\mu^-$ channel and $10^{-22}$ cm$^3$/s for the $b\bar b$ channel. For the same mass, we constrain the lifetime of dark matter to be larger than $10^{28}$ s for all channels studied, except for decaying exclusively to $b\bar b$ where it is bounded to be larger than $10^{27}$ s. Finally, we also search for evidence of astrophysical neutrinos scattering on galactic dark matter in two scenarios. For fermionic dark matter with a vector mediator, we constrain the dimensionless coupling associated with this interaction to be less than 0.1 for dark matter mass of 0.1 GeV and a mediator mass of $10^{-4}~$ GeV. In the case of scalar dark matter with a fermionic mediator, we constrain the coupling to be less than 0.1 for dark matter and mediator masses below 1 MeV.