Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Aartsen, M. G.; Abbasi, Rasha; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Altmann, D.; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; Baker, M.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Tjus, J. Becker; Becker, K. H.; 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.; Bose, D.; Böser, S.; Botner, O.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Bruijn, R.; Casey, J.; Casier, M.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Classen, L.; Clevermann, F.; Coenders, S.; Cohen, S.; Cowen, D. F.; Silva, A. H. Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Ridder, S. De; Desiati, P.; Vries, Krijn de; DeYoung, T.; Díaz-Vélez, J. C.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eichmann, B.; Eisch, J.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Franckowiak, A.; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gallagher, John S.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Goodman, J. A.; Góra, Dariusz; Grandmont, D. T.; Grant, D.; Gretskov, P.; Groh, J. C.; Groß, A.; Ha, C.; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huang, F.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Hussain, Shahid; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Jagielski, K.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Kelley, J. L.; Kiryluk, J.; Kläs, J.; Klein, S. R.; Köhne, J. H.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krasberg, M.; Kriesten, A.; Krings, K.; Kroll, G.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Landsman, H.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leute, J.; Lünemann, J.; Macías, Óscar; Madsen, J.; Maggi, G.; Maruyama, R.; Mase, K.; Matis, H. S.; McNally, F.; Meagher, K.; Merck, M.; Meures, T.; Miarecki, S.; Middell, E.; Milke, N.; Miller, J.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, Uwe; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Odrowski, S.; Olivas, A.; Omairat, A.; O’Murchadha, A.; Palczewski, T.; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Quinnan, M.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Reimann, R.; Resconi, E.; Rhode, W.; Ribordy, M.; Richman, M.; Riedel, Benedikt; Robertson, S.; Rodrigues, J. P.; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Sander, H. G.; Santander, M.; Sarkar, S.; Schatto, K.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Sestayo, Y.; Seunarine, S.; Shanidze, R.; Sheremata, C.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Tepe, A.; Ter–Antonyan, S.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toscano, S.; Tselengidou, M.; Unger, E.; Usner, M.; Vallecorsa, S.; Eijndhoven, N. van; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.; Ziemann, J.; Zierke, S.; Zoll, M.

doi:10.1103/physrevd.89.062007

Cited by 102 publications

(112 citation statements)

References 50 publications

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“…The expected number of events in bin i, m i , is given by the sum of the four flux expectations for the conventional, isotropic astrophysical, prompt, and Galactic flux: Here x conv and x prompt refer to nuisance parameters, taking into account the theoretical uncertainties on the respective fluxes. The atmospheric neutrino fluxes have been corrected for the cosmicray knee following the prescription in Aartsen et al (2014a). We include nuisance parameters that account for the choice of the primary cosmic-ray model and uncertainties in the cosmic-ray spectral index.…”

Section: Diffuse-template Analysismentioning

confidence: 99%

Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data

Aartsen¹,

Ackermann²,

Adams³

et al. 2017

ApJ

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132

117

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The origins of high-energy astrophysical neutrinos remain a mystery despite extensive searches for their sources. We present constraints from seven years of IceCube Neutrino Observatory muon data on the neutrino flux coming from the Galactic plane. This flux is expected from cosmic-ray interactions with the interstellar medium or near localized sources. Two methods were developed to test for a spatially extended flux from the entire plane, both of which are maximum likelihood fits but with different signal and background modeling techniques. We consider three templates for Galactic neutrino emission based primarily on gamma-ray observations and models that cover a wide range of possibilities. Based on these templates and in the benchmark case of an unbroken E − 2.5 power-law energy spectrum, we set 90% confidence level upper limits, constraining the possible Galactic contribution to the diffuse neutrino flux to be relatively small, less than 14% of the flux reported in Aartsen et al. above 1 TeV. A stacking method is also used to test catalogs of known high-energy Galactic gamma-ray sources.

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Section: Diffuse-template Analysismentioning

confidence: 99%

Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data

Aartsen¹,

Ackermann²,

Adams³

et al. 2017

ApJ

Self Cite

132

117

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“…In two of these -IC40 and IC59 -slight excesses of neutrino events at the highest energies were seen, hinting at the existence of a diffuse astrophysical flux. The IC40 analysis [19] looked for shower-like events, and the IC59 analysis [20] measured track events from muon neutrinos. These two analyses yielded excesses with significances of 2.7σ and 1.8σ respectively -too small to be considered as evidence for a real signal, but, nonetheless, excesses of events above…”

Section: Hints Of An Astrophysical Diffuse Flux Signalmentioning

confidence: 99%

First detection of high-energy astrophysical neutrinos with IceCube

2015

AIP Conference Proceedings

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“…This data set consists of approximately 22 000 up-going track-like events from chargedcurrent muon neutrino interactions that have good reconstruction quality and energies between about 100 GeV and 50 TeV. For details about the event selection, see [6]. A second independent IceCube analysis of comparable sensitivity is close to completion, using the first year of data taken with the final 86-string configuration, and will be reported soon.…”

Section: The Icecube Neutrino Observatorymentioning

confidence: 99%

Search for sterile neutrinos with the IceCube Neutrino Observatory

Wallraff¹,

Wiebusch²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The IceCube Neutrino Observatory is a 1 km 3 Cherenkov detector located at the geographic South Pole. It records several tens of thousands high-energy atmospheric muon neutrino events per year, with energies between about one hundred GeV and several tens of TeV. This allows a precise measurement of the energy and angular distributions and a search for deviations from the standard expectation that could be due to new physics. If additional sterile neutrino states exist with mass differences on the order of 1 eV and mix with muon neutrinos, IceCube would observe a deficit compared to the expected neutrino rate in the energy range of a few TeV due to strong matter effects in the neutrino propagation through Earth. The disappearance depends on the energy and the path of the neutrino through the Earth and thus its zenith angle. Here, we report on the first exploratory effort to make use of this resonance effect to substantially improve the sensitivity with respect to searches that are based on vacuum oscillations. This paper describes results that are based on a large muon neutrino sample measured by IceCube between 2009 and 2010 in its 59-string configuration.

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Search for a diffuse flux of astrophysical muon neutrinos with the IceCube 59-string configuration

Cited by 102 publications

References 50 publications

Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data

Constraints on Galactic Neutrino Emission with Seven Years of IceCube Data

First detection of high-energy astrophysical neutrinos with IceCube

Search for sterile neutrinos with the IceCube Neutrino Observatory

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