The IceCube Neutrino Observatory - Contributions to ICRC 2015 Part II: Atmospheric and Astrophysical Diffuse Neutrino Searches of All Flavors

Aartsen, M. G.; Abraham, K.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, W. G.; Ansseau, I.; Archinger, M.; Argüelles, Carlos; Arlen, T. C.; Auffenberg, J.; Bai, X.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, Julia Becker; Becker, K.-H.; Beiser, E.; BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Böhm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz, H.-P.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Cowen, D. F.; Silva, A. H. Cruz; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Rosendo, E. del Pino; Dembinski, H.-P.; Ridder, S. De; Desiati, P.; Vries, Krijn de; Wasseige, Gwenhaël de; DeYoung, Tyce; Díaz–Vélez, Juan Carlos; Lorenzo, V. di; Dumm, J.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Ehrhardt, Thomas; Eichmann, B.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fahey, S.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Fösig, C.-C.; Fuchs, T.; Gaisser, T. K.; Gaïor, R.; Gallagher, John S.; Gerhardt, L.; Ghorbani, K.; Gier, D.; Gladstone, L.; Glagla, M.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Góra, Dariusz; Grant, D.; Groh, J. C.; Groß, A.; Ha, C.; Haack, Christian; Ismail, A. Haj; Hallgren, A.; Halzen, F.; Hansmann, B.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Holzapfel, Killian; Homeier, A.; Hoshina, K.; Huang, F.; Huber, Matthías; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jero, K.; Jurković, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kemp, J.; Kheirandish, Ali; Kiryluk, J.; Kläs, J.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Konietz, R.; Koob, A.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leuner, J.; Lu, Lina; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, Kendall; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli, A.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Middell, E.; Middlemas, E.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Olivas, A.; Omairat, A.; O’Murchadha, A.; Palczewski, T.; Pandya, Hershal; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Pütz, J.; Quinnan, M.; Raab, Christoph; Rädel, L.; Rameez, M.; Rawlins, K.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Richter, S.; Riedel, Benedikt; Robertson, Sally; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Saba, S. M.; Sabbatini, L.; Sander, H.G.; Sandrock, A.; Sandroos, J.; Sarkar, Subir; Schatto, K.; Scheriau, F.; Schimp, Michael; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schulte, L.; Seckel, D.; Seunarine, S.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, C.; Stahlberg, M.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola, H.; Taboada, I.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tosi, D.; Tselengidou, M.; Turcati, A.; Unger, E.; Usner, M.; Vallecorsa, S.; Vandenbroucke, J.; Eijndhoven, N. van; Vanheule, S.; Santen, J. V.; Veenkamp, J.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandkowsky, N.; Weaver, Ch.; Wendt, Chris; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wichary, C.; Wiebe, K.; Wiebusch, Christopher; Wille, L.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zoll, M.

doi:10.48550/arxiv.1510.05223

Cited by 71 publications

(187 citation statements)

References 2 publications

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“…More precisely, comparing the flux obtained fitting the passing muons with the flux obtained fitting the HESE seen from the Southern sky results in a much greater tension. In [17] the flux of diffuse astrophysical muon is analyzed and it is found α p = 1.91 ± 0.20 for the spectral index. This flux is obtained using events in the energy range between 170 TeV and 3.8 PeV, but if the single power law hypothesis is the true one this flux must be valid also at lower energies.…”

Section: Comparison Of the Power Law Distributions Obtained From Diff...mentioning

confidence: 99%

Extragalactic Plus Galactic Model for Icecube Neutrino Events

Palladino

Vissani

2016

ApJ

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The hypothesis that high-energy cosmic neutrinos are power law distributed is critically analyzed. We propose a model with two components that better explains the observations. The extragalactic component of the high-energy neutrino flux has a canonical n -E 2 spectrum while the galactic component has a n -E 2.7 spectrum; both of them are significant. This model has several implications, which can be tested by IceCube and ANTARES over the next several years. Moreover, the existence of a diffuse component, close to the Galactic plane and that yields (20-30)% of IceCube's events, is interesting for the future km 3 neutrino telescopes located in the Northern Hemisphere and for gamma-ray telescopes aiming to measure events up to a few 100 TeV from the southern sky.

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Section: Comparison Of the Power Law Distributions Obtained From Diff...mentioning

confidence: 99%

Extragalactic Plus Galactic Model for Icecube Neutrino Events

Palladino

Vissani

2016

ApJ

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“…N → W ± ∓ . This raises the interesting possibility of explaining the IceCube PeV neutrinos 32 when we set M N ∼ few PeV. 15 However, the two-body decays are disfavored by the IceCube data, as the neutrino spectrum is flatter than required.…”

Section: Decaying Rhn Dm and Icecube Pev Neutrinosmentioning

confidence: 99%

Heavy right-handed neutrino dark matter in left–right models

Dev

Mohapatra

2017

Mod. Phys. Lett. A

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We show that in a class of non-supersymmetric left-right extensions of the Standard Model (SM), the lightest right-handed neutrino (RHN) can play the role of thermal Dark Matter (DM) in the Universe for a wide mass range from TeV to PeV. Our model is based on the gauge groupwhich a heavy copy of the SM fermions are introduced and the stability of the RHN DM is guaranteed by an automatic Z 2 symmetry present in the leptonic sector. In such models the active neutrino masses are obtained via the type-II seesaw mechanism. We find a lower bound on the RHN DM mass of order TeV from relic density constraints, as well as an unitarity upper bound in the multi-TeV to PeV scale, depending on the entropy dilution factor. The RHN DM could be made long-lived by soft-breaking of the Z 2 symmetry and provides a concrete example of decaying DM interpretation of the PeV neutrinos observed at IceCube.

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“…We present an update to the selection and analysis of IceCube's High Energy Starting Events (HESE), a sample of high energy neutrinos with interaction vertices contained within the detector fiducial volume. Previously this sample was analyzed with two [1], three [2], four [3], and six [4] years of data, leading to the discovery of a high-energy astrophysical neutrino flux. This work extends the sample with an additional one and a half years of data for a total of 2635 days of livetime, but primarily improves the description of atmospheric background and the treatment of uncertainties.…”

Section: Introductionmentioning

confidence: 99%

Characterization of the Astrophysical Diffuse Neutrino Flux with IceCube High-Energy Starting Events

Schneider¹

2019

Preprint

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The IceCube neutrino observatory has established the existence of an astrophysical diffuse neutrino component above ∼ 100 TeV. This discovery was made using the high-energy starting event sample, which uses the outer layer of instrumented volume as a veto to significantly reduce atmospheric background. We present the latest astrophysical neutrino flux measurement using highenergy starting events. This latest iteration of the analysis extends the sample by 1.5 years for a total of 7.5 years, updates the event properties with newer models of light transport in the glacial ice, and has an improved systematic treatment. As part of this new analysis, we report on compatibility of our observations with detailed isotropic flux models proposed in the literature as well as the standard generic models such as single, double power-law scenarios. We find that none of the tested models are substantially preferred with respect to a single power law.

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The IceCube Neutrino Observatory - Contributions to ICRC 2015 Part II: Atmospheric and Astrophysical Diffuse Neutrino Searches of All Flavors

Cited by 71 publications

References 2 publications

Extragalactic Plus Galactic Model for Icecube Neutrino Events

Extragalactic Plus Galactic Model for Icecube Neutrino Events

Heavy right-handed neutrino dark matter in left–right models

Characterization of the Astrophysical Diffuse Neutrino Flux with IceCube High-Energy Starting Events

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