Measurement of South Pole ice transparency with the IceCube LED calibration system

Aartsen, M. G.; Abbasi, Rasha; Abdou, Y.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Altmann, D.; Auffenberg, J.; Bai, X.; Baker, M. D.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Bechet, S.; Tjus, J. Becker; Becker, K. H.; Bell, Michael; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, Jens; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Bertrand, Daniel; Besson, D.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohaichuk, S.; Böhm, C.; Bose, D.; Böser, S.; Botner, O.; Brayeur, L.; Brown, A. M.; Bruijn, R.; Brünner, J.; Buitink, S.; Carson, M.; Casey, J.; Casier, M.; Chirkin, D.; Christy, B.; Clark, K.; Clevermann, F.; Cohen, S.; Cowen, D. F.; Silva, A.H. Cruz; Danninger, M.; Daughhetee, J.; Davis, J.; Clercq, C. De; Ridder, S. De; Desiati, P.; With, M. de; DeYoung, T.; Díaz-Vélez, J. C.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eisch, J.; Ellsworth, R. W.; 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.; Franke, Robert; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; Goodman, J. A.; Góra, Dariusz; Grant, D.; Groß, A.; Gurtner, M.; Ha, C.; Ismail, A. Haj; Hallgren, A.; Halzen, F.; Hanson, K.; Heereman, D.; Heimann, P.; Heinen, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Homeier, A.; Hoshina, K.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; Hussain, Safeer; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Japaridze, G. S.; Jero, K.; Jlelati, O.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kelley, J. L.; Kiryluk, J.; Kislat, Fabian; 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.; Kroll, G.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Landsman, H.; Larson, M. J.; Lesiak-Bzdak, M.; Leute, J.; Lünemann, J.; Madsen, J.; Maruyama, R.; Mase, K.; Matis, H. S.; McNally, F.; Meagher, K.; Merck, M.; Mészáros, P.; 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.; Olivo, M.; O’Murchadha, A.; Paul, Larissa; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pirk, Norbert; Posselt, J.; Price, P. B.; Przybylski, G. T.; Rädel, L.; Rawlins, K.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Richman, M.; Riedel, Benedikt; Rodrigues, J. P.; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Salameh, T.; Sander, H. G.; Santander, M.; Sarkar, S.; Schatto, K.; Scheel, Mark A.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönherr, L.; Schönwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Seo, S. h.; Sestayo, Y.; Seunarine, S.; Sheremata, C.; Smith, M. W. E.; Soiron, M.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stößl, A.; Strahler, E. A.; Strom, Lars Rickard; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Ter–Antonyan, S.; Tilav, S.; Toale, P. A.; Toscano, S.; Usner, M.; Drift, D. van der; Eijndhoven, N. van; Overloop, A. Van; Santen, J. V.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Wasserman, R.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Xu, C.; Xu, Dawei; Xu, X. W.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Zarzhitsky, P.; Ziemann, J.; Zierke, S.; Zilles, Anne; Zoll, M.

doi:10.1016/j.nima.2013.01.054

Cited by 165 publications

(199 citation statements)

References 12 publications

(36 reference statements)

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“…The IceCube ice model applied in this analysis has nearly a thousand free parameters that are minimized in an iterative fit procedure using light-emitting diode flasher data [60]. The model implements vertically varying absorption and scattering coefficients across tilted isochronal ice layers.…”

Section: Prl 117 071801 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 99%

Searches for Sterile Neutrinos with the IceCube Detector

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Phys. Rev. Lett.

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240

350

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The IceCube neutrino telescope at the South Pole has measured the atmospheric muon neutrino spectrum as a function of zenith angle and energy in the approximate 320 GeV to 20 TeV range, to search for the oscillation signatures of light sterile neutrinos. No evidence for anomalous $\nu_\mu$ or $\bar{\nu}_\mu$ disappearance is observed in either of two independently developed analyses, each using one year of atmospheric neutrino data. New exclusion limits are placed on the parameter space of the 3+1 model, in which muon antineutrinos would experience a strong MSW-resonant oscillation. The exclusion limits extend to $\mathrm{sin}^2 2\theta_{24} \leq$ 0.02 at $\Delta m^2 \sim$ 0.3 $\mathrm{eV}^2$ at the 90\% confidence level. The allowed region from global analysis of appearance experiments, including LSND and MiniBooNE, is excluded at approximately the 99\% confidence level for the global best fit value of $|$U$_{e4}|^2$.Comment: 10 pages, 5 figure

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Section: Prl 117 071801 (2016) P H Y S I C a L R E V I E W L E T T Ementioning

confidence: 99%

Searches for Sterile Neutrinos with the IceCube Detector

Aartsen¹,

Abraham²,

Ackermann³

et al. 2016

Phys. Rev. Lett.

Self Cite

240

350

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show abstract

“…Neutrino induced muons are then tracked into and through the detector taking account of stochastic and continuous energy losses [25]. Cherenkov light from charged particles is propagated to the optical modules [26] taking account of scattering and absorption in the ice [27,28]. Finally, the generation of the signal as a function of time in the optical module is simulated in detail.…”

Section: Fig 1 (Color Online)mentioning

confidence: 99%

“…(iv) Optical properties of Antarctic ice Photons produced by secondary particles in the detection volume are subject to scattering and absorption during propagation to the DOMs. The optical properties of the Antarctic ice have been estimated using calibration light sources inside the ice following two approaches [27,28] and show a spatial dependence in particular in the vertical direction. The influence on the observables due to both ice models (SPICE Mie, WHAM!)…”

Section: A Neutrino Detection Uncertainties (I) Optical Efficiency Omentioning

confidence: 99%

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

Aartsen¹,

Abbasi²,

Ackermann³

et al. 2014

Phys. Rev. D

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102

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when the array was running in its 59-string configuration. The data sample was optimized to contain muon neutrino induced events with a background contamination of atmospheric muons of less than 1%. These data, which are dominated by atmospheric neutrinos, are analyzed with a global likelihood fit to search for possible contributions of prompt atmospheric and astrophysical neutrinos, neither of which have yet been identified. Such signals are expected to follow a harder energy spectrum than conventional atmospheric neutrinos. In addition, the zenith angle distribution differs for astrophysical and atmospheric signals. A global fit of the reconstructed energies and directions of observed events is performed, including possible neutrino flux contributions for an astrophysical signal and atmospheric backgrounds as well as systematic uncertainties of the experiment and theoretical predictions. The best fit yields an astrophysical signal flux for ν μ þν μ of E 2 · ΦðEÞ ¼ 0.25 × 10 −8 GeV cm −2 s −1 sr −1 ,

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“…The characteristics of the ice were examined using LEDs installed in DOM. The revised ice model with a new simulation describes more precisely our observational data [6].…”

Section: Introductionmentioning

confidence: 98%

The Latest IceCube Results and the Implications

Mase¹

2017

Proceedings of the 7th International Workshop on Very High Energy Particle Astronomy in 2014 (VHEPA2014)

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IceCube was built at the South Pole and aims to detect high energy neutrinos from the universe mainly above 100 GeV. The transparent ice media allows us to build a 1 km 3 large detection volume to detect the rarely interacting particles. Neutrinos are thought to be generated at astrophysical sources such as active galactic nuclei and gamma-ray bursts. Nature of the rare interaction with matters and little deflection by a magnetic field makes it possible to explore such sources located at the deep universe. Since the neutrinos are produced through collisions of hadronic particles, the observation can elucidate the origin of cosmic rays, which is still mystery after the discovery 100 years ago. The detector was completed at the end of 2010 and is running smoothly. Recently, IceCube has found the first evidence of extraterrestrial neutrinos with energies above approximately 60 TeV. IceCube also contributes to elementary particle physics by searching for neutrinos produced in self-annihilation of SUSY particles such as neutralinos and by investigating atmospheric neutrino oscillations. The latest IceCube results and the corresponding implications are presented.

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Measurement of South Pole ice transparency with the IceCube LED calibration system

Cited by 165 publications

References 12 publications

Searches for Sterile Neutrinos with the IceCube Detector

Searches for Sterile Neutrinos with the IceCube Detector

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

The Latest IceCube Results and the Implications

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