Determining neutrino oscillation parameters from atmospheric muon neutrino disappearance with three years of IceCube DeepCore data

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, W. G.; Argüelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; 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.; Bos, F.; Bose, D.; Boeser, S.; Botner, O.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Brünner, J.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Classen, L.; Clevermann, F.; Coenders, S.; Cowen, D. F.; Silva, A. H. Cruz; Daughhetee, J.; Davis, J.; Day, M.; André, J. P. A. M. de; Clercq, C. De; Ridder, S. De; Desiati, P.; Vries, Krijn de; Young, T.; Díaz–Vélez, Juan Carlos; Dunkman, M.; Eagan, R.; Eberhardt, B.; Eichmann, B.; Eisch, J.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, Anatoli; Feintzeig, J.; Felde, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Franckowiak, A.; Frantzen, K.; Fuchs, T.; Gaisser, T. K.; Gaïor, R.; Gallagher, John S.; Gerhardt, L.; Gier, D.; Gladstone, L.; Gluesenkamp, T.; Goldschmidt, A.; Golup, G.; González, J. G.; Goodman, J. A.; Góra, D.; Grant, D.; Gretskov, P.; Groh, J. C.; Groß, A.; Ha, C.; Haack, Christian; Ismail, A. Haj; Hallen, P.; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Heinen, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; 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.; Jurković, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, Ali; Kiryluk, J.; Klaes, Jonas; Klein, S. R.; Koehne, J. H.; Kohnen, G.; Kolanoski, H.; Koob, A.; Koepke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Kriesten, A.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larsen, D.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Luenemann, J.; Madsen, J.; Maggi, G.; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli, A.; Meures, T.; Miarecki, S.; Middell, E.; Middlemas, 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; Penek, Ö.; Pepper, J. A.; Heros, C. Pérez de los; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Puetz, J.; Quinnan, M.; Raedel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Rees, I.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Riedel, Benedikt; Robertson, Sally; Rodrigues, J. P.; Rongen, Martin; Rott, C.; Ruhe, T.; Ruzybayev, B.; Ryckbosch, D.; Saba, S. M.; Sander, H. G.; Sandroos, J.; Santander, M.; Sarkar, S.; Schatto, K.; Scheriau, F.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schoeneberg, S.; Schoenwald, A.; Schukraft, A.; Schulte, L.; Schulz, O.; Seckel, D.; Sestayo, Y.; Seunarine, S.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, Christian; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stoeßl, A.; Strahler, E. A.; Strom, Lars Rickard; Strotjohann, N. L.; Sullivan, G. W.; Taavola, H.; Taboada, I.; Tamburro, A.; Tepe, A.; Ter–Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tosi, D.; Tselengidou, M.; Unger, E.; Usner, M.; Vallecorsa, S.; Eijndhoven, N. van; Vandenbroucke, J.; Santen, J. V.; Vehring, M.; Vöge, M.; Vraeghe, M.; Walck, C.; Wallraff, M.; Weaver, Ch.; Wellons, M.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wichary, C.; 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.91.072004

Cited by 138 publications

(178 citation statements)

References 42 publications

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“…Most works in the literature have focused on the capabilities of past and current [31-39, 41, 44-46, 48, 49] or future detectors [40-43, 45, 47, 50] using atmospheric neutrino events in the O(10 GeV) energy range, where interference effects may take place. In particular, the Super-Kamiokande (SK) collaboration (exploiting the sub-GeV, multi-GeV, stopping and through-going muon samples) obtained the most stringent bounds on the diagonal and off-diagonal NSI parameters in the µτ -sector [39,46] and recently, the IceCube Collaboration has also presented a preliminary analysis [49] using the DeepCore three-year muon disappearance result [51], with slightly more restrictive limits than SK.…”

Section: Jhep01(2017)141mentioning

confidence: 99%

Non-standard interactions with high-energy atmospheric neutrinos at IceCube

Salvadó

Mena

Palomares‐Ruiz

et al. 2017

J. High Energ. Phys.

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Non-standard interactions in the propagation of neutrinos in matter can lead to significant deviations from expectations within the standard neutrino oscillation framework and atmospheric neutrino detectors have been considered to set constraints. However, most previous works have focused on relatively low-energy atmospheric neutrino data. Here, we consider the one-year high-energy through-going muon data in IceCube, which has been already used to search for light sterile neutrinos, to constrain new interactions in the µτ -sector. In our analysis we include several systematic uncertainties on both, the atmospheric neutrino flux and on the detector properties, which are accounted for via nuisance parameters. After considering different primary cosmic-ray spectra and hadronic interaction models, we improve over previous analysis by using the latest data and showing that systematics currently affect very little the bound on the off-diagonal ε µτ , with the 90% credible interval given by −6.0 × 10 −3 < ε µτ < 5.4 × 10 −3 , comparable to previous results. In addition, we also estimate the expected sensitivity after 10 years of collected data in IceCube and study the precision at which non-standard parameters could be determined for the case of ε µτ near its current bound.

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Section: Jhep01(2017)141mentioning

confidence: 99%

Non-standard interactions with high-energy atmospheric neutrinos at IceCube

Salvadó

Mena

Palomares‐Ruiz

et al. 2017

J. High Energ. Phys.

View full text Add to dashboard Cite

show abstract

“…Denoting with Y χ = n χ /s the DM abundance, where n χ is the number density of the DM particles and s = 2π 2 45 g * (T )T 3 the entropy density (g * denotes the degrees of freedom), from the Boltzmann equation one gets…”

Section: Pev Neutrinos and Ice Cube Datamentioning

confidence: 99%

“…2 Investigations along these lines have been performed in different cosmological scenarios [63][64][65][66][67][68][69][70][71][72], where The parameter ν labels cosmological models: ν = 2 in Randall-Sundrum type II brane cosmology [73], ν = 1 in kination models [74][75][76][77], ν = 0 in cosmologies with an overall boost of the Hubble expansion rate [63], ν = − 0.8 in scalar-tensor cosmology [63,78], ν = 2/n − 2 in f (R) cosmology, with f (R) = R + α R n [79,80]. In terms of the modified expansion rate (3.2), it then follows that the inverse decay processes (2.6) takes the form…”

Section: Pev Neutrinos In Modified Cosmologiesmentioning

confidence: 99%

“…In the form (4.2), the STT action is refereed as Jordan frame. By means of the conformal transformationg μν = A C (φ)g μν (A C is the conformal factor that depends on φ(x)) and setting 2 …”

Section: Scalar Tensor Theories (Stts)mentioning

confidence: 99%

“…The IceCube Collaboration, in its 4-year dataset [1,2], had reported three neutrino-induced cascade events with energies ∼ 1 PeV [2]. First candidates for the generation of such neutrino high energy events were various astrophysical sources [3][4][5][6].…”

Section: Introductionmentioning

confidence: 99%

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PeV IceCube signals and Dark Matter relic abundance in modified cosmologies

2018

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The discovery by the IceCube experiment of a high-energy astrophysical neutrino flux with energies of the order of PeV, has opened new scenarios in astroparticles physics. A possibility to explain this phenomenon is to consider the minimal models of Dark Matter (DM) decay, the 4-dimensional operator ∼ y αχ L L α H χ , which is also able to generate the correct abundance of DM in the Universe. Assuming that the cosmological background evolves according to the standard cosmological model, it follows that the rate of DM decay χ ∼ |y αχ | 2 needed to get the correct DM relic abundance ( χ ∼ 10 −58 ) differs by many orders of magnitude with respect that one needed to explain the IceCube data ( χ ∼ 10 −25 ), making the four-dimensional operator unsuitable. In this paper we show that assuming that the early Universe evolution is governed by a modified cosmology, the discrepancy between the two the DM decay rates can be reconciled, and both the IceCube neutrino rate and relic density can be explained in a minimal model.

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Joint $$\nu $$ + $$\bar{\nu }$$ Oscillation Analysis: Results

Duffy

2017

First Measurement of Neutrino and Antineutrino Oscillation at T2K

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Determining neutrino oscillation parameters from atmospheric muon neutrino disappearance with three years of IceCube DeepCore data

Cited by 138 publications

References 42 publications

Non-standard interactions with high-energy atmospheric neutrinos at IceCube

Non-standard interactions with high-energy atmospheric neutrinos at IceCube

PeV IceCube signals and Dark Matter relic abundance in modified cosmologies

Joint $$\nu $$ + $$\bar{\nu }$$ Oscillation Analysis: Results

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