The IceCube Neutrino Observatory - Contributions to ICRC 2017 Part II: Properties of the Atmospheric and Astrophysical Neutrino Flux

Aartsen, M. G.; Eijndhoven, N. van; Meagher, K.; Huang, Feng; Pandya, H.; Kim, J.; Yodh, G.; Kunwar, S.; Collin, Gabriel; Stettner, J.; Micallef, Jessie; Cross, R.; Lauber, Frederik Hermann; Jones, B. J. P.; Lesiak-Bzdak, M.; Vries, Krijn de; Sandrock, A.; Gerhardt, L.; Westerhoff, S.; Wandkowsky, N.; Wallraff, M.; Bradascio, Federica; Day, M.; Mase, K.; Meier, Maximilian; Waza, A.; Sarkar, Subir; Hignight, J.; Schumacher, Lisa Johanna; Blot, Summer; Hoffman, K. D.; Yañez, J. P.; Kolanoski, H.; Steuer, A.; Cowen, D. F.; Mahn, Kendall; Friedman, E.; Braun, J.; Wills, L.; Tatar, J.; Kalaczyński, P.; Nahnhauer, R.; Relethford, B.; Pinat, E.; Spiczak, G. M.; Labare, M.; BenZvi, S.; Stachurska, J.; Halzen, F.; Glauch, Theo; Desiati, P.; Eller, P.; González, J. G.; Berley, D.; Pepper, J. A.; Koirala, R.; Rawlins, K.; Sutherland, M.; Stasik, A.; Whelan, B. J.; Andeen, K.; Bagherpour, H.; Filimonov, K.; DeLaunay, James; Fuchs, T.; Ty, Bunheng; Stößl, A.; Song, M.; Neer, G.; Liu, Q.R.; Rameez, M.; Xu, X. W.; Clercq, C. De; McNally, F.; Anderson, W. G.; Gallagher, John S.; Hünnefeld, Mirco; Larson, M. J.; Haack, Christian; Glüsenkamp, T.; Hickford, S.; Ryckbosch, D.; Vogel, E.; Luszczak, William; Hoffmann, R.; In, S.; Casey, J.; Wendt, Chris; Wasseige, Gwenhaël de; Ahlers, M.; Pieloth, D.; Palczewski, T.; Kunnen, J.; Heereman, D.; Samarai, I. Al; Jacobi, E.; Montaruli, T.; Brenzke, M.; Naumann, Uwe; Williams, D.; Botner, O.; Unger, E.; Woolsey, E.; Dembinski, H.-P.; Burgman, A.; Stezelberger, T.; Maruyama, R.; Hill, G. C.; Rysewyk, D.; Lanfranchi, J. L.; Casier, M.; Maunu, R.; Rhode, W.; Tjus, Julia Becker; Börner, M.; O’Murchadha, A.; Classen, L.; Tosi, D.; Woschnagg, K.; Nygren, D. R.; Griffith, Z.; Hanson, K.; Santen, J. V.; Clark, K.; Finley, C.; Satalecka, K.; Hebecker, D.; Grant, D.; Kintscher, T.; Chirkin, D.; Tobin, M. N.; Medici, M.; Schoenen, S.; Argüelles, C.; Wiebe, K.; Weiss, Matthew J.; Robertson, S.; Rea, Immacolata Carmen; Koskinen, D. J.; Giang, W.; Franckowiak, A.; Nowicki, S. C.; Vraeghe, M.; Huber, Matthías; Menne, T.; Ghorbani, K.; Yoshida, Shigeru; Kappes, A.; Jeong, Minjin; Köpke, L.; Christov, A.; Niederhausen, H.; Kyriacou, A.; Sandroos, J.; Momenté, G.; Toscano, S.; Felde, J.; Hultqvist, K.; Karg, T.; Bourbeau, J.; Kiryluk, J.; Tselengidou, M.; Eberhardt, B.; Brostean-Kaiser, Jannes; Kopper, C.; Kopper, S.; Koschinsky, J. P.; Böhm, C.; Bron, S.; Werthebach, Johannes; Meures, T.; Wandler, F. D.; Bay, R.; Katz, U.; Dunkman, M.; Yuan, Tianlu; Adams, J.; Nakarmi, P.; Coenders, S.; Karle, A.; Heros, C. Pérez de los; Aguilar, J. A.; Goldschmidt, A.; Díaz-Vélez, J.C.; Moulai, Marjon; Pankova, D. V.; Kowalski, M.; Fahey, S.; Taboada, I.; Stamatikos, M.; Ackermann, M.; Anton, Gisela; Kheirandish, Ali; Axani, Spencer; Hallgren, A.; Wood, J.; Soedingrekso, Jan; Becker, Karl‐Heinz; Krings, K.; Driessche, W. Van; Zoll, M.; Baum, V.; Turley, C. F.; Mancina, Sarah; Blaufuss, E.; Ahrens, M.; Bos, F.; Xu, Dawei; Rott, C.; Soldin, D.; Fazely, A. R.; Gaisser, T. K.; Usner, M.; Sälzer, T.; Hellauer, R.; Wallace, A.; Böser, S.; Wood, T. R.; Bernardini, E.; Stanev, T.; Barron, J. P.; Altmann, D.; Beatty, J. J.; Merino, G.; Kim, M.; Besson, D.; Binder, G.; Ehrhardt, Thomas; Bose, D.; Conrad, J. M.; DeYoung, Tyce; Ansseau, I.; Bai, X.; Hoshina, K.; Walck, C.; Kohnen, G.; Toale, P. A.; Leuermann, M.; Bindig, D.; Rongen, Martin; Herrera, S. E. Sanchez; Flis, S.; Kelley, J. L.; Seunarine, S.; Tešić, G.; Moore, R.; Ter–Antonyan, S.; Turcati, A.; Klein, S. R.; Spiering, C.; Japaridze, G. S.; Kurahashi, N.; Helbing, K.; Tenholt, F.; Miarecki, S.; Vandenbroucke, J.; Vanheule, S.; Sullivan, G. W.; Wickmann, S.; Kauer, M.; Lu, Lina; Terliuk, A.; Ridder, S. De; Przybylski, G. T.; Brayeur, L.; Madsen, J.; Evenson, P. A.; Eichmann, B.; Kittler, T.; Wiebusch, C. H.; Relich, M.; Kuwabara, T.; Ruhe, T.; Cheung, E.; Xu, Y.; Plum, M.; Tilav, S.; Kang, W.; Lünemann, J.; Weaver, C.; Barwick, S. W.; Tung, Chun Fai; Strotjohann, N. L.; Rädel, L.; Schmidt, T.; Jero, K.; Olivas, A.; Auffenberg, J.; Peiffer, P.; Schlunder, P.; Kroll, M.; Wolf, M.; Raab, Christoph; Dujmović, Hrvoje; Schöneberg, S.; Keivani, A.; Lorenzo, V. di; Price, P. Buford; Richman, M.; Resconi, E.; Maggi, G.; Pollmann, A. Obertacke; Ishihara, A.; Schneider, A.; Seckel, D.; Bretz, H.-P.; André, J. P. A. M. de; Lennarz, D.; Krückl, G.; Reimann, R.; Hokanson-Fasig, B.; Carver, T.; Stokstad, R.G.; Dumm, J.; Wille, L.; Vehring, M.

doi:10.48550/arxiv.1710.01191

Cited by 92 publications

(218 citation statements)

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“…22 The energy spectrum of E −2.5 agrees with the measurement using upgoing muons with a spectral index of E −2.4 above an energy of ∼ 100 TeV. 12 In general, analyses reaching lower energies exhibit larger spectral indices with the updated 7.5 years starting-event sample, 19 yielding a spectral index value of −2.87 ± 0.2 for the 68.3% confidence interval.…”

Section: Neutrinos Interacting Inside the Instrumented Volumesupporting

confidence: 66%

“…Muon neutrinos can be detected even when interacting outside the detector because of the kilometer range of the secondary muons. More importantly, IceCube has observed an excess of neutrino events at energies beyond 100 TeV [10][11][12] that cannot be accounted for by the atmospheric flux at the 5.6σ level. A recent…”

Section: Muon Neutrinos Through the Earthmentioning

confidence: 99%

“…The present seven-year data set contains a total of 60 neutrino events with deposited energies ranging from 60 TeV to 10 PeV that are likely to be of cosmic origin. The deposited energy and zenith dependence of the high-energy starting events 12,19 is compared to the atmospheric background in Fig. 6.…”

Section: Neutrinos Interacting Inside the Instrumented Volumementioning

confidence: 99%

“…Left Panel: Deposited energies, by neutrinos interacting inside IceCube, observed in six years of data. 12 The grey region shows uncertainties on the sum of all backgrounds. The atmospheric muon flux (blue) and its uncertainty is computed from simulation to overcome statistical limitations in our background measurement and scaled to match the total measured background rate.…”

Section: Future Plansmentioning

confidence: 99%

See 3 more Smart Citations

The Observation of High-Energy Neutrinos from the Cosmos: Lessons Learned for Multimessenger Astronomy

Halzen

2021

Preprint

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The IceCube neutrino telescope discovered PeV-energy neutrinos originating beyond our Galaxy with an energy flux that is comparable to that of GeV-energy gamma rays and EeV-energy cosmic rays. These neutrinos provide the only unobstructed view of the cosmic accelerators that power the highest energy radiation reaching us from the universe. We will review the results from IceCube's first decade of operations, emphasizing the measurement of the diffuse multiflavored neutrino flux from the universe and the identification of the supermassive black hole TXS 0506+056 as a source of cosmic neutrinos and, therefore, cosmic rays. We will speculate on the lessons learned for multimessenger astronomy, among them that extragalactic neutrino sources may be a relatively small subset of the cosmic accelerators observed in high-energy gamma rays and that these may be gamma-ray-obscured at the times that they emit neutrinos.

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Section: Neutrinos Interacting Inside the Instrumented Volumesupporting

confidence: 66%

Section: Muon Neutrinos Through the Earthmentioning

confidence: 99%

Section: Neutrinos Interacting Inside the Instrumented Volumementioning

confidence: 99%

Section: Future Plansmentioning

confidence: 99%

See 2 more Smart Citations

The Observation of High-Energy Neutrinos from the Cosmos: Lessons Learned for Multimessenger Astronomy

Halzen

2021

Preprint

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“…The 1 km 3 IceCube neutrino telescope [8] has collected large samples of neutrino events, sometimes comprising more than 500,000 neutrino events [9]. Optical sensors observe the Cherenkov radiation from relativistic charged particles produced in the interactions.…”

Section: Introductionmentioning

confidence: 99%

Nuclear effects in high-energy neutrino interactions

Klein,

Robertson,

Vogt

2020

Preprint

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Neutrino telescopes like IceCube, KM3NeT and Baikal-GVD offer physicists the opportunity to study neutrinos with energies far beyond the reach of terrestrial accelerators. These neutrinos are used to study high-energy neutrino interactions and to probe the Earth through absorption tomography. Current studies of TeV neutrinos use cross sections which are calculated for free nucleons with targets which are assumed to contain equal numbers of protons and neutrons.Here we consider modifications of high-energy neutrino interactions due to two nuclear effects: modifications of the parton densities in the nucleus, referred to here as shadowing, and the effect of non-isoscalar targets, with unequal numbers of neutrons and protons. Both these effects depend on the interaction medium. Because shadowing is larger for heavier nuclei, such as iron, found in the Earth's core, it introduces a zenith-angle dependent change in the absorption cross section. These modifications increase the cross sections by 1-2% at energies below 100 TeV (antishadowing), and reduce it by 3-4% at higher energies (shadowing).Nuclear effects also alter the inelasticity distribution of neutrino interactions in water/ice by increasing the number of low inelasticity interactions, with a larger effect for ν than ν. These effects are particularly large in the energy range below a few TeV. These effects could alter the cross sections inferred from events with tracks originating within the active detector volume as well as the ratio ν/ν inferred from inelasticity measurements.The uncertainties in these nuclear effects are larger than the uncertainties on the free-proton cross sections and will thus limit the systematic precision of future high-precision measurements at neutrino telescopes.

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Interactions of astrophysical neutrinos with dark matter: a model building perspective

Pandey

Karmakar

Rakshit

2019

J. High Energ. Phys.

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We explore the possibility that high energy astrophysical neutrinos can interact with the dark matter on their way to Earth. Keeping in mind that new physics might leave its signature at such energies, we have considered all possible topologies for effective interactions between neutrino and dark matter. Building models, that give rise to a significant flux suppression of astrophysical neutrinos at Earth, is rather difficult. We present a Z -mediated model in this context. Encompassing a large variety of models, a wide range of dark matter masses from 10 −21 eV up to a TeV, this study aims at highlighting the challenges one encounters in such a model building endeavour after satisfying various cosmological constraints, collider search limits and electroweak precision measurements. *

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The IceCube Neutrino Observatory - Contributions to ICRC 2017 Part II: Properties of the Atmospheric and Astrophysical Neutrino Flux

Cited by 92 publications

References 0 publications

The Observation of High-Energy Neutrinos from the Cosmos: Lessons Learned for Multimessenger Astronomy

The Observation of High-Energy Neutrinos from the Cosmos: Lessons Learned for Multimessenger Astronomy

Nuclear effects in high-energy neutrino interactions

Interactions of astrophysical neutrinos with dark matter: a model building perspective

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