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Search for neutrino-induced particle showers with IceCube-40

(2014) PHYSICAL REVIEW D. 89(10).
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IceCube
Abstract
We report on the search for neutrino-induced particle showers, so-called cascades, in the IceCube-40 detector. The data for this search were collected between April 2008 and May 2009 when the first 40 IceCube strings were deployed and operational. Three complementary searches were performed, each optimized for different energy regimes. The analysis with the lowest energy threshold (2 TeV) targeted atmospheric neutrinos. A total of 67 events were found, consistent with the expectation of 41 atmospheric muons and 30 atmospheric neutrino events. The two other analyses targeted a harder, astrophysical neutrino flux. The analysis with an intermediate threshold of 25 TeV leads to the observation of 14 cascadelike events, again consistent with the prediction of 3.0 atmospheric neutrino and 7.7 atmospheric muon events. We hence set an upper limit of E-2 Phi(lim) <= 7.46 x 10(-8) GeV sr(-1) s(-1) cm(-2) (90% C.L.) on the diffuse flux from astrophysical neutrinos of all neutrino flavors, applicable to the energy range 25 TeV to 5 PeV, assuming an E-nu(-2) spectrum and a neutrino flavor ratio of 1: 1: 1 at the Earth. The third analysis utilized a larger and optimized sample of atmospheric muon background simulation, leading to a higher energy threshold of 100 TeV. Three events were found over a background prediction of 0.04 atmospheric muon events and 0.21 events from the flux of conventional and prompt atmospheric neutrinos. Including systematic errors this corresponds to a 2.7 sigma excess with respect to the background-only hypothesis. Our observation of neutrino event candidates above 100 TeV complements IceCube's recently observed evidence for high-energy astrophysical neutrinos.
Keywords
SCATTERING, SELECTION, CASCADES, SPECTRUM, AMANDA, SYSTEM, MODEL, ICE

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Citation

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

Chicago
Aartsen, MG, R Abbasi, M Ackermann, J Adams, JA Aguilar, M Ahlers, D Altmann, et al. 2014. “Search for Neutrino-induced Particle Showers with IceCube-40.” Physical Review D 89 (10).
APA
Aartsen, M., Abbasi, R., Ackermann, M., Adams, J., Aguilar, J., Ahlers, M., Altmann, D., et al. (2014). Search for neutrino-induced particle showers with IceCube-40. PHYSICAL REVIEW D, 89(10).
Vancouver
1.
Aartsen M, Abbasi R, Ackermann M, Adams J, Aguilar J, Ahlers M, et al. Search for neutrino-induced particle showers with IceCube-40. PHYSICAL REVIEW D. 2014;89(10).
MLA
Aartsen, MG, R Abbasi, M Ackermann, et al. “Search for Neutrino-induced Particle Showers with IceCube-40.” PHYSICAL REVIEW D 89.10 (2014): n. pag. Print.
@article{4432811,
  abstract     = {We report on the search for neutrino-induced particle showers, so-called cascades, in the IceCube-40 detector. The data for this search were collected between April 2008 and May 2009 when the first 40 IceCube strings were deployed and operational. Three complementary searches were performed, each optimized for different energy regimes. The analysis with the lowest energy threshold (2 TeV) targeted atmospheric neutrinos. A total of 67 events were found, consistent with the expectation of 41 atmospheric muons and 30 atmospheric neutrino events. The two other analyses targeted a harder, astrophysical neutrino flux. The analysis with an intermediate threshold of 25 TeV leads to the observation of 14 cascadelike events, again consistent with the prediction of 3.0 atmospheric neutrino and 7.7 atmospheric muon events. We hence set an upper limit of E-2 Phi(lim) {\textlangle}= 7.46 x 10(-8) GeV sr(-1) s(-1) cm(-2) (90\% C.L.) on the diffuse flux from astrophysical neutrinos of all neutrino flavors, applicable to the energy range 25 TeV to 5 PeV, assuming an E-nu(-2) spectrum and a neutrino flavor ratio of 1: 1: 1 at the Earth. The third analysis utilized a larger and optimized sample of atmospheric muon background simulation, leading to a higher energy threshold of 100 TeV. Three events were found over a background prediction of 0.04 atmospheric muon events and 0.21 events from the flux of conventional and prompt atmospheric neutrinos. Including systematic errors this corresponds to a 2.7 sigma excess with respect to the background-only hypothesis. Our observation of neutrino event candidates above 100 TeV complements IceCube's recently observed evidence for high-energy astrophysical neutrinos.},
  articleno    = {102001},
  author       = {Aartsen, MG and Abbasi, R and Ackermann, M and Adams, J and Aguilar, JA and Ahlers, M and Altmann, D and Arguelles, C and Arlen, TC and Auffenberg, J and Bai, X and Baker, M 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 Bose, D and Boser, S and Botner, O and Brayeur, L and Bretz, HP and Brown, AM and Bruijn, R and Casey, J and Casier, M and Chirkin, D and Christov, A and Christy, B and Clark, K and Classen, L and Clevermann, F and Coenders, S and Cohen, S and Cowen, DF and Silva, AHC and Danninger, M and Daughhetee, J and Davis, JC and Day, M and de Andre, JPAM and De Clercq, C and De Ridder, Sam and Desiati, P and de Vries, KD and de With, M and DeYoung, T and Diaz-Velez, JC and Dunkman, M and Eagan, R and Eberhardt, B 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 Feusels, Tom and Filimonov, K and Finley, C and Fischer-Wasels, T and Flis, S and Franckowiak, A and Frantzen, K and Fuchs, T and Gaisser, TK and Gallagher, J and Gerhardt, L and Gladstone, L and Glusenkamp, T and Goldschmidt, A and Golup, G and Gonzalez, JG and Goodman, JA and Gora, D and Grandmont, DT and Grant, D and Gretskov, P and Groh, JC and Gross, A and Ha, 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 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 Hussain, S and Ishihara, A and Jacobi, E and Jacobsen, J and Jagielski, K and Japaridze, GS and Jero, K and Jlelati, Ola and Kaminsky, B and Kappes, A and Karg, T and Karle, A and Kauer, M and Kelley, JL and Kiryluk, J and Klas, J and Klein, SR and Kohne, JH and Kohnen, G and Kolanoski, H and Kopke, L and Kopper, C and Kopper, S and Koskinen, DJ and Kowalski, M and Krasberg, M and Kriesten, A and Krings, K and Kroll, G and Kunnen, J and Kurahashi, N and Kuwabara, T and Labare, Mathieu and Landsman, H and Larson, MJ and Lesiak-Bzdak, M and Leuermann, M and Leute, J and Lunemann, J and Macias, O and Madsen, J and Maggi, G and Maruyama, R and Mase, K and Matis, HS and McNally, F and Meagher, K and Merck, M and Meures, T and Miarecki, S and Middell, 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 Odrowski, S and Olivas, A and Omairat, A and O'Murchadha, A and Palczewski, T and Paul, L and Pepper, JA and de los Heros, CP and Pfendner, C and Pieloth, D and Pinat, E and Posselt, J and Price, PB and Przybylski, GT and Quinnan, M and Radel, L and Rameez, M and Rawlins, K and Redl, P and Reimann, R and Resconi, E and Rhode, W and Ribordy, M and Richman, M and Riedel, B and Robertson, S and Rodrigues, JP and Rott, C and Ruhe, T and Ruzybayev, B and Ryckbosch, Dirk and Saba, SM and Sander, HG and Santander, M and Sarkar, S and Schatto, K and Scheriau, F and Schmidt, T and Schmitz, M and Schoenen, S and Schoneberg, S and Schonwald, A and Schukraft, A and Schulte, L and Schulz, O and Seckel, D and Sestayo, Y and Seunarine, S and Shanidze, R and Sheremata, C 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 Stossl, A and Strahler, EA and Strom, R and Strotjohann, NL and Sullivan, GW and Taavola, H and Taboada, I and Tamburro, A and Tepe, A and Ter-Antonyan, S and Tesic, G and Tilav, S and Toale, PA and Tobin, MN and Toscano, S and Tselengidou, M and Unger, E and Usner, M and Vallecorsa, S and van Eijndhoven, N and Van Overloop, Arne and van Santen, J and Vehring, M and Voge, M and Vraeghe, Matthias and Walck, C and Waldenmaier, T and Wallraff, M and Weaver, C and Wellons, M and Wendt, C and Westerhoff, S and Whelan, B and Whitehorn, N 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 Yanez, JP and Yodh, G and Yoshida, S and Zarzhitsky, P and Ziemann, J and Zierke, S and Zoll, M},
  issn         = {1550-7998},
  journal      = {PHYSICAL REVIEW D},
  keyword      = {SCATTERING,SELECTION,CASCADES,SPECTRUM,AMANDA,SYSTEM,MODEL,ICE},
  language     = {eng},
  number       = {10},
  pages        = {20},
  title        = {Search for neutrino-induced particle showers with IceCube-40},
  url          = {http://dx.doi.org/10.1103/PhysRevD.89.102001},
  volume       = {89},
  year         = {2014},
}

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