Search for dark matter from the Galactic halo with the IceCube Neutrino Telescope

Abbasi, Rasha; Abdou, Y.; Abu‐Zayyad, T.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Bay, R.; Alba, J. L. Bazo; Beattie, K.; Beatty, J. J.; Bechet, S.; Becker, J.; Becker, K. H.; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, Daniel; Besson, D.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, C.; Bose, D.; Boeser, S.; Botner, O.; Braun, J.; Brown, A. M.; Buitink, S.; Carson, M.; Chirkin, D.; Christy, B.; Clem, J.; Clevermann, F.; Cohen, S.; Colnard, C.; Cowen, D. F.; D’Agostino, M. V.; Danninger, M.; Daughhetee, J.; Davis, J.; Clercq, C. De; Demiroers, L.; Denger, T.; Depaepe, O.; Descamps, F.; Desiati, P.; Vries-Uiterweerd, G. de; DeYoung, T.; Díaz–Vélez, Juan Carlos; Dierckxsens, M.; Dreyer, J.; Dumm, J. P.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Engdegård, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, Robert; Gaisser, T. K.; Gallagher, J.; Geisler, M.; Gerhardt, L.; Gladstone, L.; Gluesenkamp, T.; Goldschmidt, A.; Goodman, J. A.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Heinen, D.; Helbing, K.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Homeier, A.; Hoshina, K.; Hubert, D.; Huelsnitz, W.; Huelss, J. P.; Hulth, P. O.; Hultqvist, K.; Hussain, Shahid; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Joseph, J.; Kampert, K.‐H.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kenny, Patrick; Kiryluk, J.; Kislat, Fabian; Klein, S. R.; Koehne, J. H.; Kohnen, G.; Kolanoski, H.; Koepke, L.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Krings, T.; Kroll, G.; Kuêhn, K.; Kuwabara, T.; Labare, M.; Lafèbre, S.; Laihem, K.; Landsman, H.; Larson, M. J.; Lauer, R.; Luenemann, J.; Madsen, J.; Majumdar, P.; Marotta, Anna; Maruyama, R.; Mase, K.; Matis, H. S.; Meagher, K.; Merck, M.; Mészáros, P.; Meures, T.; Middell, E.; Milke, N.; Miller, J.; Montaruli, T.; Morse, R.; Movit, S. M.; Nahnhauer, R.; Nam, J. W.; Naumann, Uwe; Nießen, P.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; O’Murchadha, A.; Ono, M.; Panknin, S.; Paul, Larissa; Heros, C. Pérez de los; Petrović, J.; Piegsa, A.; Pieloth, D.; Porrata, R.; Posselt, J.; Price, P. B.; Prikockis, M.; Przybylski, G. T.; Rawlins, K.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Rodrigues, J. P.; Roth, Peter M.; Rothmaier, F.; Rott, C.; Ruhe, T.; Rutledge, D.; Ruzybayev, B.; Ryckbosch, D.; Sander, H. G.; Santander, M.; Sarkar, S.; Schatto, K.; Schmidt, T.; Schoenwald, A.; Schukraft, A.; Schultes, A.; Schulz, O.; Schunck, M.; Seckel, D.; Semburg, B.; Seo, S. h.; Cerra, Yolanda Sestayo de la; Seunarine, S.; Silvestri, A.; Slipak, A.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stephens, G.; Stezelberger, T.; Stokstad, R. G.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Stüer, M.; Sullivan, G. W.; Swillens, Q.; Taavola, H.; Taboada, I.; Tamburro, A.; Tarasova, O.; Tepe, A.; Ter–Antonyan, S.; Tilav, S.; Toale, P. A.; Toscano, S.; Tosi, D.; Turčan, D.; Eijndhoven, N. van; Vandenbroucke, J.; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Voigt, B.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Walter, Michael; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Wolf, M.; Woschnagg, K.; Xu, C.; Xu, X. W.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.

doi:10.1103/physrevd.84.022004

Cited by 114 publications

(145 citation statements)

References 59 publications

(65 reference statements)

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“…J → W W, ZZ that could be induced in some UV-completions of our model. We stress, however, that J → νν could still be an important discovery channel for majoron masses up to 10 TeV, for which IceCube becomes the ideal observatory [63,64]. The neutrino (plus antineutrino) flux per flavor from the J → νν decay in our galaxy is given by [26,65] …”

Section: Neutrino Signaturesmentioning

confidence: 90%

Neutrino lines from majoron dark matter

Garcia-Cely

Heeck

2017

J. High Energ. Phys.

101

151

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Models with spontaneously broken global lepton number can lead to a pseudoGoldstone boson as a long-lived dark matter candidate. Here we revisit the case of singlet majoron dark matter and discuss multiple constraints. For masses above MeV, this model could lead to a detectable flux of monochromatic mass-eigenstate neutrinos, which have flavor ratios that depend strongly on the neutrino mass hierarchy. We provide a convenient parametrization for the loop-induced majoron couplings to charged fermions that allows us to discuss three-generation effects such as lepton flavor violation. These couplings are independent of the low-energy neutrino parameters but can be constrained by the majoron decays into charged fermions.

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Section: Neutrino Signaturesmentioning

confidence: 90%

Neutrino lines from majoron dark matter

Garcia-Cely

Heeck

2017

J. High Energ. Phys.

101

151

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“…Also, in this context, some have considered the isotropic arrival directions of cosmic neutrinos to be a clue that they originate in the Galactic halo as a result of the decay of PeV-energy dark matter particles, a speculation that at this point is perfectly consistent with observations [33][34][35][36][37][38][39][40] . More traditionally, IceCube searches for dark matter by looking for the annihilation of weakly interacting massive particles (WIMPs) wherever they have accumulated to a high density: in the Sun 41 , in the Milky Way 42,43 , and in nearby galaxies 44 . For instance, WIMPs are swept up by the Sun as the solar system moves about the galactic halo.…”

Section: High-energy Neutrinos and Dark Mattermentioning

confidence: 99%

High-energy neutrino astrophysics

Halzen

2016

Nature Phys

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The chargeless, weakly interacting neutrinos are ideal astronomical messengers as they travel through space without scattering, absorption or deflection. But this weak interaction also makes them notoriously di cult to detect, leading to neutrino observatories requiring large-scale detectors. A few years ago, the IceCube experiment discovered neutrinos originating beyond the Sun with energies bracketed by those of the highest energy gamma rays and cosmic rays. I discuss how these high-energy neutrinos can be detected and what they can tell us about the origins of cosmic rays and about dark matter.

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“…Ice Cube has now reported limits on the annihilation cross section into several channels through observations of the diffuse Galactic halo with an exposure of 276 days and a 22-string configuration (Abbasi et al, 2011). For dark matter mass greater than 20 GeV, the best-constrained channel is the direct annihilation of dark matter to neutrinos, for which the limits are σ ann v 10 −22 cm 3 s −1 .…”

Section: Neutrino Searchesmentioning

confidence: 99%

Galactic searches for dark matter

2013

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For nearly a century, more mass has been measured in galaxies than is contained in the luminous stars and gas. Through continual advances in observations and theory, it has become clear that the dark matter in galaxies is not comprised of known astronomical objects or baryonic matter, and that identification of it is certain to reveal a profound connection between astrophysics, cosmology, and fundamental physics. The best explanation for dark matter is that it is in the form of a yet undiscovered particle of nature, with experiments now gaining sensitivity to the most well-motivated particle dark matter candidates. In this article, I review measurements of dark matter in the Milky Way and its satellite galaxies and the status of Galactic searches for particle dark matter using a combination of terrestrial and space-based astroparticle detectors, and large scale astronomical surveys. I review the limits on the dark matter annihilation and scattering cross sections that can be extracted from both astroparticle experiments and astronomical observations, and explore the theoretical implications of these limits. I discuss methods to measure the properties of particle dark matter using future experiments, and conclude by highlighting the exciting potential for dark matter searches during the next decade, and beyond.

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Search for dark matter from the Galactic halo with the IceCube Neutrino Telescope

Cited by 114 publications

References 59 publications

Neutrino lines from majoron dark matter

Neutrino lines from majoron dark matter

High-energy neutrino astrophysics

Galactic searches for dark matter

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