Multiyear search for a diffuse flux of muon neutrinos with AMANDA-II

Achterberg, A.; Ackermann, M.; Adams, J. H.; Ahrens, J.; Andeen, K.; Auffenberg, J.; Bai, X.; Baret, B.; Barwick, S. W.; Bay, R.; Beattie, K.; Becka, T.; Becker, J. K.; Becker, K.-H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, Daniel; Besson, D.; Blaufuss, E.; Boersma, D. J.; Böhm, C.; Bolmont, J.; Böser, S.; Botner, O.; Bouchta, A.; Braun, J.; Burgess, T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.; D’Agostino, M. V.; Davour, Anna; Day, C. T.; Clercq, C. De; Demirörs, L.; Descamps, F.; Desiati, P.; DeYoung, T.; Díaz–Vélez, Juan Carlos; Dreyer, J.; Dumm, J.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Filimonov, K.; Finley, C.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, Robert; Gaisser, T. K.; Gallagher, John S.; Ganugapati, R.; Geenen, H.; Gerhardt, L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Griesel, T.; Groß, A.; Grullon, S.; Gunasingha, R. M.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Hart, J. E.; Hasegawa, Y.; Hauschildt, T.; Hays, D.; Heise, J.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hodges, J.; Hoffman, K. D.; Hommez, B.; Hoshina, K.; Hubert, D.; Hughey, B.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Inaba, M.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Jones, Aaron; Joseph, J.; Kampert, K.‐H.; Kappes, A.; Karg, T.; Karle, A.; Kawai, H.; Kelley, J. L.; Kislat, Fabian; Kitamura, N.; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Kuêhn, K.; Labare, M.; Landsman, H.; Lauer, R.; Leich, H.; Leier, Dominik; Liubarsky, I.; Lundberg, J.; Lünemann, J.; Madsen, J.; Maruyama, R.; Mase, K.; Matis, H. S.; McCauley, T.; McParland, C.; Meli, A.; Messarius, T.; Mészáros, P.; Miyamoto, H.; Mokhtarani, A.; Montaruli, T.; Morey, A.; Morse, R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.; Öğelman, H.; Olivas, A.; Patton, S.; Peña-Garay, Carlos; Heros, C. P. L. de los; Piegsa, A.; Pieloth, D.; Pohl, A. C.; Porrata, R.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins, S.; Roth, Peter M.; Rothmaier, F.; Rott, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. G.; Sarkar, S.; Satalecka, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Seckel, D.; Semburg, B.; Seo, S. h.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Smith, A. J.; Solarz, M.; Song, Cui-Ying; Sopher, J.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K.-H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tarasova, O.; Tepe, A.; Thollander, L.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Tosi, D.; Turčan, D.; Eijndhoven, N. van; Vandenbroucke, J.; Overloop, A. Van; Viscomi, V.; Voigt, B.; Wagner, Wolfgang; Walck, C.; Waldmann, H.; Walter, Michael; Wang, Y. R.; Wendt, C.; Wiebusch, C. H.; Wiedemann, C.; Wikström, G.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, Shigeru; Zornoza, J.D.

doi:10.1103/physrevd.76.042008

Cited by 97 publications

(23 citation statements)

References 46 publications

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“…Searches for high-energy astrophysical neutrinos have been performed ever since the beginning of IceCube datataking, as before with data collected by IceCube's predecessor AMANDA (see e.g. Achterberg et al 2007;Abbasi et al 2011). Here, we consider only more recent searches, and only those targeted at the TeV-PeV energy range.…”

Section: Searches For High-energy Neutrinos With Icecubementioning

confidence: 99%

A Combined Maximum-Likelihood Analysis of the High-Energy Astrophysical Neutrino Flux Measured With Icecube

Aartsen

Abraham

Ackermann³

et al. 2015

ApJ

Self Cite

445

678

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Evidence for an extraterrestrial flux of high-energy neutrinos has now been found in multiple searches with the IceCube detector. The first solid evidence was provided by a search for neutrino events with deposited energies 30 TeV and interaction vertices inside the instrumented volume. Recent analyses suggest that the extraterrestrial flux extends to lower energies and is also visible with throughgoing, ν µ-induced tracks from the Northern hemisphere. Here, we combine the results from six different IceCube searches for astrophysical neutrinos in a maximum-likelihood analysis. The combined event sample features high-statistics samples of shower-like and track-like events. The data are fit in up to three observables: energy, zenith angle and event topology. Assuming the astrophysical neutrino flux to be isotropic and to consist of equal flavors at Earth, the all-flavor spectrum with neutrino energies between 25 TeV and 2.8 PeV is well described by an unbroken power law with best-fit spectral index −2.50 ± 0.09 and a flux at 100 TeV of 6.7 +1.1 −1.2 • 10 −18 GeV −1 s −1 sr −1 cm −2. Under the same assumptions, an unbroken power law with index −2 is disfavored with a significance of 3.8 σ (p = 0.0066%) with respect to the best fit. This significance is reduced to 2.1 σ (p = 1.7%) if instead we compare the best fit to a spectrum with index −2 that has an exponential cutoff at high energies. Allowing the electron neutrino flux to deviate from the other two flavors, we find a ν e fraction of 0.18 ± 0.11 at Earth. The sole production of electron neutrinos, which would be characteristic of neutron-decay dominated sources, is rejected with a significance of 3.6 σ (p = 0.014%).

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Section: Searches For High-energy Neutrinos With Icecubementioning

confidence: 99%

A Combined Maximum-Likelihood Analysis of the High-Energy Astrophysical Neutrino Flux Measured With Icecube

Aartsen

Abraham

Ackermann³

et al. 2015

ApJ

Self Cite

445

678

View full text Add to dashboard Cite

show abstract

“…The blue triangles are the result from an independent unfolding analysis of IceCube 40 string data (Abbasi et al, 2010a). For comparison several experimental limits (Abbasi et al, 2009d(Abbasi et al, , 2010bAchterberg et al, 2007;Anton, 2010) and theoretical flux predictions for atmospheric (Barr et al, 2004;Enberg et al, 2008;Fiorentini et al, 2001;Honda et al, 2007) and astrophysical (Becker et al, 2005;Mannheim, 1995;Mücke et al, 2003;Razzaque et al, 2003;Stecker, 2005;Bahcall, 1997, 1998) neutrinos are given.…”

Section: Randd Activitiesmentioning

confidence: 99%

The IceCube neutrino observatory: Status and initial results

Karg

2010

Preprint

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The IceCube collaboration is building a cubic kilometer scale neutrino telescope at a depth of 2km at the geographic South Pole, utilizing the clear Antarctic ice as a Cherenkov medium to detect cosmic neutrinos. The Ice-Cube observatory is complemented by IceTop, a square kilometer air shower array on top of the in-ice detector. The construction of the detector is nearly finished with 79 of a planned 86 strings and 73 of 80 IceTop stations deployed. Its completion is expected in the winter 2010/11. Using data from the partially built detector, we present initial results of searches for neutrinos from astrophysical sources such as supernova remnants, active galactic nuclei, and gamma ray bursts, for anisotropies in cosmic rays, and constraints on the dark matter scattering cross section. Further, we discuss future plans and R&D activities towards new neutrino detection techniques.

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“…. Line 2 is for Amanda II within 807 days observation [22]. Line 5 is for IceCube with three year of observation [27].…”

Section: Sensitivitymentioning

confidence: 99%

Simulation of the cosmic ray tau neutrino telescope (CRTNT) experiment

Liu¹,

Zhang²,

Cao³

et al. 2009

J. Phys. G: Nucl. Part. Phys.

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A τ lepton can be produced in a charged current interaction by cosmic ray tau neutrino with material inside a mountain. If it escapes from the mountain, it will decay and initiate a shower in the air, which can be detected by an air shower fluorescence/Cherenkov light detector. Designed according to such a principle, the Cosmic Ray Tau Neutrino Telescope (CRTNT) experiment, located at the foothill of Mt. Balikun in Xinjiang, China, will search for very high-energy cosmic τ neutrinos from energetic astrophysical sources by detecting those showers. This paper describes a Monte Carlo simulation for a detection of τ events by the CRTNT experiment. Ultra-high-energy cosmic ray events are also simulated to estimate the potential contamination. With the CRTNT experiment composed of four detector stations, each covering 64 • × 14 • field of view, the expected event rates are 28.6, 21.9 and 4.7 per year assuming AGN neutrino flux according to Semikoz et. al. 2004, MPR AGN jet model and SDSS AGN core model, respectively. Null detection of such τ event by the CRTNT experiment in one year could set 90% C.L. upper limit at 19.9(eV · cm −2 · s −1 · sr −1 ) for E −2 neutrino spectrum.PACS numbers: 96.85. Ry, 96.40.Pq, 98.70.Sa, 95.55.Vj

show abstract

Multiyear search for a diffuse flux of muon neutrinos with AMANDA-II

Cited by 97 publications

References 46 publications

A Combined Maximum-Likelihood Analysis of the High-Energy Astrophysical Neutrino Flux Measured With Icecube

A Combined Maximum-Likelihood Analysis of the High-Energy Astrophysical Neutrino Flux Measured With Icecube

The IceCube neutrino observatory: Status and initial results

Simulation of the cosmic ray tau neutrino telescope (CRTNT) experiment

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