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Flavor ratio of astrophysical neutrinos above 35 TeV in IceCube

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iceCube
Abstract
A diffuse flux of astrophysical neutrinos above 100 TeV has been observed at the IceCube Neutrino Observatory. Here we extend this analysis to probe the astrophysical flux down to 35 TeV and analyze its flavor composition by classifying events as showers or tracks. Taking advantage of lower atmospheric backgrounds for showerlike events, we obtain a shower-biased sample containing 129 showers and 8 tracks collected in three years from 2010 to 2013. We demonstrate consistency with the (f(e) : f(mu) : f(tau))(circle plus) approximate to (1 : 1 : 1)(circle plus) flavor ratio at Earth commonly expected from the averaged oscillations of neutrinos produced by pion decay in distant astrophysical sources. Limits are placed on nonstandard flavor compositions that cannot be produced by averaged neutrino oscillations but could arise in exotic physics scenarios. A maximally tracklike composition of (0 : 1 : 0)(circle plus) is excluded at 3.3 sigma, and a purely showerlike composition of (1 : 0 : 0)(circle plus) is excluded at 2.3 sigma.
Keywords
ACCELERATION, FLUX, COSMIC-RAYS, AMANDA, ENERGIES

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Citation

Please use this url to cite or link to this publication:

Chicago
Aartsen, MG, M Ackermann, J Adams, JA Aguilar, M Ahlers, M Ahrens, D Altmann, et al. 2015. “Flavor Ratio of Astrophysical Neutrinos Above 35 TeV in IceCube.” Physical Review Letters 114 (17).
APA
Aartsen, M., Ackermann, M., Adams, J., Aguilar, J., Ahlers, M., Ahrens, M., Altmann, D., et al. (2015). Flavor ratio of astrophysical neutrinos above 35 TeV in IceCube. PHYSICAL REVIEW LETTERS, 114(17).
Vancouver
1.
Aartsen M, Ackermann M, Adams J, Aguilar J, Ahlers M, Ahrens M, et al. Flavor ratio of astrophysical neutrinos above 35 TeV in IceCube. PHYSICAL REVIEW LETTERS. 2015;114(17).
MLA
Aartsen, MG, M Ackermann, J Adams, et al. “Flavor Ratio of Astrophysical Neutrinos Above 35 TeV in IceCube.” PHYSICAL REVIEW LETTERS 114.17 (2015): n. pag. Print.
@article{5981019,
  abstract     = {A diffuse flux of astrophysical neutrinos above 100 TeV has been observed at the IceCube Neutrino Observatory. Here we extend this analysis to probe the astrophysical flux down to 35 TeV and analyze its flavor composition by classifying events as showers or tracks. Taking advantage of lower atmospheric backgrounds for showerlike events, we obtain a shower-biased sample containing 129 showers and 8 tracks collected in three years from 2010 to 2013. We demonstrate consistency with the (f(e) : f(mu) : f(tau))(circle plus) approximate to (1 : 1 : 1)(circle plus) flavor ratio at Earth commonly expected from the averaged oscillations of neutrinos produced by pion decay in distant astrophysical sources. Limits are placed on nonstandard flavor compositions that cannot be produced by averaged neutrino oscillations but could arise in exotic physics scenarios. A maximally tracklike composition of (0 : 1 : 0)(circle plus) is excluded at 3.3 sigma, and a purely showerlike composition of (1 : 0 : 0)(circle plus) is excluded at 2.3 sigma.},
  articleno    = {171102},
  author       = {Aartsen, MG and Ackermann, M and Adams, J and Aguilar, JA and Ahlers, M and Ahrens, M and Altmann, D and Anderson, T and Arguelles, C and Arlen, TC and Auffenberg, J and Bai, X and Barwick, SW and Baum, V and Bay, R and Beatty, JJ and Tjus, JB and Becker, KH and BenZvi, S and Berghaus, P and Berley, D and Bernardini, E and Bernhard, A and Besson, DZ and Binder, G and Bindig, D and Bissok, M and Blaufuss, E and Blumenthal, J and Boersma, DJ and Bohm, C and Bos, F and B{\"o}ser, D and Botner, O and Brayeur, L and Bretz, HP and Brown, AM and Buzinsky, N and Casey, J and Casier, M and Cheung, E and Chirkin, D and Christov, A and Christy, B and Clark, K and Classen, L and Clevermann, F and Coenders, S and Cowen, DF and Silva, AHC and Daughhetee, J and Davis, JC and Day, M and de Andr{\'e}, JPAM and De Clercq, C and Dembinski, H and De Ridder, Sam and Desiati, P and de Vries, KD and de With, M and De Young, T and D{\'i}az-V{\'e}lez, JC and Dumm, JP and Dunkman, M and Eagan, R and Eberhardt, B and Ehrhardt, T and Eichmann, B and Eisch, J and Euler, S and Evenson, PA and Fadiran, O and Fazely, AR and Fedynitch, A and Feintzeig, J and Felde, J and Filimonov, K and Finley, C and Fischer-Wasels, T and Flis, S and Frantzen, K and Fuchs, T and Gaisser, TK and Gaior, R and Gallagher, J and Gerhardt, L and Gier, D and Gladstone, L and Gl{\"u}senkamp, T and Goldschmidt, A and Golup, G and Gonzalez, JG and Goodman, JA and G{\'o}ra, D and Grant, D and Gretskov, P and Groh, JC and Gross, A and Ha, C and Haack, C and Haj Ismail, Abd Al Karim and Hallen, P and Hallgren, A and Halzen, F and Hanson, K and Hebecker, D and Heereman, D and Heinen, D and Helbing, K and Hellauer, R and Hellwig, D and Hickford, S and Hill, GC and Hoffman, KD and Hoffmann, R and Homeier, A and Hoshina, K and Huang, F and Huelsnitz, W and Hulth, PO and Hultqvist, K and Ishihara, A and Jacobi, E and Jacobsen, J and Japaridze, GS and Jero, K and Jurkovic, M and Kaminsky, B and Kappes, A and Karg, T and Karle, A and Kauer, M and Keivani, A and Kelley, JL and Kheirandish, A and Kiryluk, J and Kl{\"a}s, J and Klein, SR and K{\"o}hne, JH and Kohnen, G and Kolanoski, H and Koob, A and K{\"o}pke, L and Kopper, C and Kopper, S and Koskinen, DJ and Kowalski, M and Kriesten, A and Krings, K and Kroll, G and Kroll, M and Kunnen, J and Kurahashi, N and Kuwabara, T and Labare, Mathieu and Lanfranchi, JL and Larsen, DT and Larson, MJ and Lesiak-Bzdak, M and Leuermann, M and L{\"u}nemann, J and Madsen, J and Maggi, G and Maruyama, R and Mase, K and Matis, HS and Maunu, R and McNally, F and Meagher, K and Medici, M and Meli, Athina and Meures, T and Miarecki, S and Middell, E and Middlemas, E and Milke, N and Miller, J and Mohrmann, L and Montaruli, T and Morse, R and Nahnhauer, R and Naumann, U and Niederhausen, H and Nowicki, SC and Nygren, DR and Obertacke, A and Olivas, A and Omairat, A and O'Murchadha, A and Palczewski, T and Paul, L and Penek, {\"O} and Pepper, JA and P{\'e}rez de los Heros, C and Pfendner, C and Pieloth, D and Pinat, E and Posselt, J and Price, PB and Przybylski, GT and P{\"u}tz, J and Quinnan, M and R{\"a}del, L and Rameez, M and Rawlins, K and Redl, P and Rees, I and Reimann, R and Relich, M and Resconi, E and Rhode, W and Richman, M and Riedel, B and Robertson, S and Rodrigues, JP and Rongen, M and Rott, C and Ruhe, T and Ruzybayev, B and Ryckbosch, Dirk and Saba, SM and Sander, HG and Sandroos, J and Santander, M and Sarkar, S and Schatto, K and Scheriau, F and Schmidt, T and Schmitz, M and Schoenen, S and Sch{\"o}neberg, S and Sch{\"o}nwald, A and Schukraft, A and Schulte, L and Schulz, O and Seckel, D and Sestayo, Y and Seunarine, S and Shanidze, R and Smith, MWE and Soldin, D and Spiczak, GM and Spiering, C and Stamatikos, M and Stanev, T and Stanisha, NA and Stasik, A and Stezelberger, T and Stokstad, RG and St{\"o}ssl, A and Strahler, EA and Str{\"o}m, R and Strotjohann, NL and Sullivan, GW and Taavola, H and Taboada, I and Tamburro, A and Ter-Antonyan, S and Terliuk, A and Te\v{s}i\'{c}, G and Tilav, S and Toale, PA and Tobin, MN and Tosi, D and Tselengidou, M and Unger, E and Usner, M and Vallecorsa, S and van Eijndhoven, N and Vandenbroucke, J and van Santen, J and Vanheule, Sander and Vehring, M and Voge, M and Vraeghe, Matthias and Walck, C and Wallraff, M and Weaver, C and Wellons, M and Wendt, C and Westerhoff, S and Whelan, BJ and Whitehorn, N and Wichary, C and Wiebe, K and Wiebusch, CH and Williams, DR and Wissing, H and Wolf, M and Wood, TR and Woschnagg, K and Xu, DL and Xu, XW and Xu, Y and Yanez, JP and Yodh, G and Yoshida, S and Zarzhitsky, P and Ziemann, J and Zoll, M},
  issn         = {0031-9007},
  journal      = {PHYSICAL REVIEW LETTERS},
  language     = {eng},
  number       = {17},
  pages        = {8},
  title        = {Flavor ratio of astrophysical neutrinos above 35 TeV in IceCube},
  url          = {http://dx.doi.org/10.1103/PhysRevLett.114.171102},
  volume       = {114},
  year         = {2015},
}

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