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arxiv: 2508.18103 · v2 · pith:IPKJ2HTUnew · submitted 2025-08-25 · ✦ hep-ex · hep-ph

Searching non-standard interactions with atmospheric neutrinos at ESSnuSB

ESSnuSB: J. Aguilar , M. Anastasopoulos , D. Bar\v{c}ot , E. Baussan , A. K. Bhattacharyya , A. Bignami , M. Blennow , M. Bogomilov
show 84 more authors
B. Bolling E. Bouquerel F. Bramati A. Branca G. Brunetti I. Bustinduy C. J. Carlile J. Cederkall T. W. Choi S. Choubey P. Christiansen M. Collins E. Cristaldo Morales P. Cupia{\l} D. D'Ago H. Danared J. P. A. M. de Andr\'e M. Dracos I. Efthymiopoulos T. Ekel\"of M. Eshraqi G. Fanourakis A. Farricker E. Fasoula T. Fukuda N. Gazis Th. Geralis M. Ghosh A. Giarnetti G. Gokbulut C. Hagner L. Hali\'c M. Hooft K. E. Iversen N. Jachowicz M. Jensen R. Johansson E. Kasimi A. Kayis Topaksu B. Kildetoft K. Kordas B. Kova\v{c} A. Leisos A. Longhin C. Maiano S. Marangoni J. G. Marcos C. Marrelli D. Meloni M. Mezzetto N. Milas R. Moolya J. L. Mu\~noz K. Niewczas M. Oglakci T. Ohlsson M. Olveg{\aa}rd M. Pari D. Patrzalek G. Petkov Ch. Petridou P. Poussot A. Psallidas F. Pupilli D. Saiang D. Sampsonidis A. Scanu C. Schwab F. Sordo G. Stavropoulos R. Tarkeshian F. Terranova T. Tolba E. Trachanas R. Tsenov A. Tsirigotis S. E. Tzamarias M. Vanderpoorten G. Vankova-Kirilova N. Vassilopoulos S. Vihonen J. Wurtz V. Zeter O. Zormpa
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Pith reviewed 2026-05-21 23:24 UTC · model grok-4.3

classification ✦ hep-ex hep-ph
keywords non-standard interactionsatmospheric neutrinosneutrino oscillationsESSnuSBmatter effectsmass orderingtheta23 octant
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The pith

ESSnuSB could constrain non-standard neutrino interactions using atmospheric neutrinos to levels below 0.06 at 90% CL.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper examines the capability of the ESSnuSB far detector to study non-standard neutrino interactions through atmospheric neutrino oscillations. It calculates projected upper bounds on several NSI parameters based on an exposure of 5.4 Mt·year. The study also demonstrates that these interactions can modify the experiment's sensitivity to the neutrino mass ordering and the octant of θ23. The work stresses the complementary role of atmospheric neutrino data alongside accelerator neutrinos in the ESSnuSB program.

Core claim

By analyzing atmospheric neutrino samples equivalent to 5.4 Mt·year exposure, ESSnuSB could set the upper bounds |ε_eμ^m| < 0.053, |ε_eτ^m| < 0.057, |ε_μτ^m| < 0.021, ε_ee^m - ε_μμ^m < 0.075 and |ε_ττ^m - ε_μμ^m| < 0.031 at 90% CL, when the results are minimized for the NSI phases and normal ordering is assumed. The presence of non-standard interactions could affect the sensitivities to neutrino mass ordering and θ23 octant in comparison to the standard interaction scheme.

What carries the argument

The modified neutrino propagation Hamiltonian in matter that includes non-standard interaction terms ε_αβ^m, which alter the effective potentials experienced by neutrinos traveling through Earth.

If this is right

  • NSI could lead to biases in the extracted values of standard parameters such as the mass ordering if not accounted for in the analysis.
  • The atmospheric channel provides bounds that are independent from those obtained with the neutrino beam from the accelerator.
  • Profiling over the NSI phases ensures the bounds are robust against possible phase-dependent cancellations in the oscillation probabilities.
  • Combining atmospheric and accelerator data at ESSnuSB would strengthen the overall constraints on both standard and non-standard neutrino physics.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • These projected bounds suggest that ESSnuSB could contribute meaningfully to global fits of NSI parameters from various neutrino sources.
  • Similar sensitivity studies at other proposed water Cherenkov detectors could yield comparable results if they achieve similar exposures.
  • The impact on mass ordering determination implies that NSI searches should be performed jointly with standard oscillation analyses to avoid misinterpretation.

Load-bearing premise

The analysis assumes normal neutrino mass ordering and minimizes over the NSI phases rather than fixing them or assuming inverted ordering.

What would settle it

Simulating the atmospheric neutrino events at ESSnuSB for 5.4 Mt·year exposure and performing a statistical fit for the NSI parameters; if the 90% CL upper limits obtained are significantly weaker than quoted due to unmodeled systematics, that would falsify the projected sensitivity.

Figures

Figures reproduced from arXiv: 2508.18103 by A. Bignami, A. Branca, A. Farricker, A. Giarnetti, A. Kayis Topaksu, A. K. Bhattacharyya, A. Leisos, A. Longhin, A. Psallidas, A. Scanu, A. Tsirigotis, B. Bolling, B. Kildetoft, B. Kova\v{c}, C. Hagner, Ch. Petridou, C. J. Carlile, C. Maiano, C. Marrelli, C. Schwab, D. Bar\v{c}ot, D. D'Ago, D. Meloni, D. Patrzalek, D. Saiang, D. Sampsonidis, E. Baussan, E. Bouquerel, E. Cristaldo Morales, E. Fasoula, E. Kasimi, ESSnuSB: J. Aguilar, E. Trachanas, F. Bramati, F. Pupilli, F. Sordo, F. Terranova, G. Brunetti, G. Fanourakis, G. Gokbulut, G. Petkov, G. Stavropoulos, G. Vankova-Kirilova, H. Danared, I. Bustinduy, I. Efthymiopoulos, J. Cederkall, J. G. Marcos, J. L. Mu\~noz, J. P. A. M. de Andr\'e, J. Wurtz, K. E. Iversen, K. Kordas, K. Niewczas, L. Hali\'c, M. Anastasopoulos, M. Blennow, M. Bogomilov, M. Collins, M. Dracos, M. Eshraqi, M. Ghosh, M. Hooft, M. Jensen, M. Mezzetto, M. Oglakci, M. Olveg{\aa}rd, M. Pari, M. Vanderpoorten, N. Gazis, N. Jachowicz, N. Milas, N. Vassilopoulos, O. Zormpa, P. Christiansen, P. Cupia{\l}, P. Poussot, R. Johansson, R. Moolya, R. Tarkeshian, R. Tsenov, S. Choubey, S. E. Tzamarias, S. Marangoni, S. Vihonen, T. Ekel\"of, T. Fukuda, Th. Geralis, T. Ohlsson, T. Tolba, T. W. Choi, V. Zeter.

Figure 1
Figure 1. Figure 1: FIG. 1. Absolute values of probability differences for the neutrino oscillation probability [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Probability difference [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Expected sensitivities to [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Sensitivity to neutrino mass ordering in presence of matter NSI parameters. For each true value, [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Effect of matter NSI parameters [PITH_FULL_IMAGE:figures/full_fig_p012_5.png] view at source ↗
read the original abstract

Atmospheric neutrinos provide a unique avenue to study neutrino interactions in matter. In this work, the prospects of constraining non-standard neutrino interactions with atmospheric neutrino oscillations are investigated for the proposed ESSnuSB far detector. By analyzing atmospheric neutrino samples equivalent to 5.4 Mt$\cdot$year exposure, it is found that ESSnuSB could be able to set the upper bounds $|\epsilon_{e\mu}^m| < 0.053, |\epsilon_{e\tau}^m| < 0.057, |\epsilon_{\mu\tau}^m| < 0.021, \epsilon_{ee}^m - \epsilon_{\mu\mu}^m < 0.075$ and $|\epsilon_{\tau\tau}^m - \epsilon_{\mu\mu}^m| < 0.031$ at $90\%$ CL, when the results are minimized for $\phi_{e\mu}^m, \phi_{e\tau}^m$ and $\phi_{\mu\tau}^m$ and normal ordering is assumed for neutrino masses. It is also shown that the presence of non-standard interactions could affect the sensitivities to neutrino mass ordering and $\theta_{23}^{}$ octant in comparison to the standard interaction scheme. The results of this work highlight the complementarity between atmospheric and accelerator neutrino programs in ESSnuSB.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript presents a sensitivity study for constraining non-standard neutrino interactions (NSI) in matter using atmospheric neutrino oscillations at the proposed ESSnuSB far detector. With an assumed exposure of 5.4 Mt·year, it reports 90% CL upper bounds on several NSI parameters (|ε_eμ^m| < 0.053, |ε_eτ^m| < 0.057, |ε_μτ^m| < 0.021, ε_ee^m - ε_μμ^m < 0.075, |ε_ττ^m - ε_μμ^m| < 0.031) obtained by profiling over the NSI phases φ_eμ^m, φ_eτ^m and φ_μτ^m under the assumption of normal neutrino mass ordering. The work also examines how NSI presence modifies the detector's sensitivity to mass ordering and θ23 octant relative to the standard interaction case, emphasizing complementarity with accelerator neutrino programs.

Significance. If the underlying simulation and statistical analysis are robustly documented, the study would usefully illustrate how atmospheric neutrinos at ESSnuSB can provide competitive constraints on matter NSI parameters and highlight the interplay between NSI and standard oscillation parameters. The explicit profiling over phases and the ordering assumption are correctly flagged as important for interpreting the quoted limits.

major comments (2)
  1. [Abstract] Abstract and analysis description: the numerical bounds are stated without any information on the Monte Carlo generator employed for atmospheric neutrino event simulation, the treatment or magnitude of systematic uncertainties, or the precise statistical method (e.g., definition of the test statistic or fitting procedure) used to extract the 90% CL limits. These omissions are load-bearing for the central claim because the quoted sensitivities cannot be independently verified or reproduced.
  2. [Results / sensitivity analysis] Results on ordering dependence: the headline limits are derived exclusively under normal ordering with profiling over the three NSI phases. Because NSI matter potentials enter the Hamiltonian with the same sign as the standard MSW term, the oscillation probabilities (and therefore the exclusion reach) change when Δm31² flips sign. No corresponding limits, Δχ² surfaces, or discussion for inverted ordering are provided, preventing the bounds from being regarded as ordering-independent.
minor comments (2)
  1. [Introduction] The notation ε^m (with superscript m) for matter NSI parameters should be defined explicitly at first use, together with the relation to the standard NSI formalism.
  2. [Simulation setup] Clarify whether the atmospheric neutrino flux model and detector response are taken from a public library or generated internally; a brief statement on the energy and zenith-angle ranges considered would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading of our manuscript and the constructive comments. We address each major comment point by point below, indicating where revisions will be made to improve clarity and completeness.

read point-by-point responses

  1. Referee: [Abstract] Abstract and analysis description: the numerical bounds are stated without any information on the Monte Carlo generator employed for atmospheric neutrino event simulation, the treatment or magnitude of systematic uncertainties, or the precise statistical method (e.g., definition of the test statistic or fitting procedure) used to extract the 90% CL limits. These omissions are load-bearing for the central claim because the quoted sensitivities cannot be independently verified or reproduced.

    Authors: We agree that the abstract would benefit from a concise mention of the simulation and analysis framework to aid immediate understanding. The full details of the Monte Carlo event generation, systematic uncertainty treatment, and the chi-squared test statistic (with profiling over nuisance parameters) are provided in Sections 3 and 4 of the manuscript. We will revise the abstract to include a brief reference to these elements and ensure the analysis description explicitly cross-references the relevant sections for reproducibility. revision: yes

  2. Referee: [Results / sensitivity analysis] Results on ordering dependence: the headline limits are derived exclusively under normal ordering with profiling over the three NSI phases. Because NSI matter potentials enter the Hamiltonian with the same sign as the standard MSW term, the oscillation probabilities (and therefore the exclusion reach) change when Δm31² flips sign. No corresponding limits, Δχ² surfaces, or discussion for inverted ordering are provided, preventing the bounds from being regarded as ordering-independent.

    Authors: We acknowledge the referee's point that the quoted limits are derived under normal ordering and that the sign of the matter potential affects the oscillation probabilities for inverted ordering. The manuscript explicitly states the normal-ordering assumption and the profiling over NSI phases. To make the results more comprehensive, we will add a discussion of the inverted-ordering case, including the corresponding 90% CL bounds and a brief comparison of the Δχ² behavior. revision: yes

Circularity Check

0 steps flagged

No circularity: standard sensitivity projection from simulated data

full rationale

The manuscript is a forward-looking sensitivity study that generates simulated atmospheric neutrino event samples for a 5.4 Mt·year exposure at the proposed ESSnuSB far detector, then performs a statistical fit (chi-squared minimization over NSI parameters with profiling over phases) to extract projected 90% CL bounds. The derivation chain consists of standard three-flavor oscillation probabilities in matter (including NSI terms in the Hamiltonian) applied to Monte Carlo data; the resulting limits are outputs of that statistical procedure, not inputs redefined as predictions. No self-definitional loop, fitted parameter renamed as prediction, or load-bearing self-citation is present. The normal-ordering assumption and phase profiling are explicit analysis choices whose impact is acknowledged, not hidden circularities. The central claim therefore remains independent of its own fitted values.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The study rests on the standard three-flavor oscillation framework plus the usual assumptions about atmospheric neutrino flux and detector response; no new particles or forces are postulated.

axioms (1)
  • domain assumption Three-flavor neutrino oscillations with standard interactions as the baseline model
    The search for NSI deviations presupposes the standard oscillation parameters and matter effects as the null hypothesis.

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Reference graph

Works this paper leans on

55 extracted references · 55 canonical work pages · 23 internal anchors

  1. [1]

    The neutrino oscillation probabilities are expressed up to first order in sinθ13 and ϵm eτcombined

    Here, ∆P NSI νe→νµ≡P NSI νe→νµ−P SI νe→νµis the difference between the oscillation probabilities derived for the matter NSI parameterϵm eτ≡|ϵm eτ|exp (−iϕm eτ), which is assumed to be a small parameter, and for standard interactions (SI). The neutrino oscillation probabilities are expressed up to first order in sinθ13 and ϵm eτcombined. An analogous expre...

    work page 2000

  2. [2]

    NuFit-6.0: Updated global analysis of three-flavor neutrino oscillations

    I. Esteban, M. C. Gonzalez-Garcia, M. Maltoni, I. Martinez-Soler, J. a. P. Pinheiro, and T. Schwetz, JHEP12, 216, arXiv:2410.05380 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  3. [3]

    Status of non-standard neutrino interactions

    T. Ohlsson, Rept. Prog. Phys.76, 044201 (2013), arXiv:1209.2710 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  4. [4]

    Neutrino oscillations and Non-Standard Interactions

    Y. Farzan and M. Tórtola, Front. in Phys.6, 10 (2018), arXiv:1710.09360 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  5. [5]

    Scalar Non-Standard Interactions in Neutrino Oscillation

    S.-F. Ge and S. J. Parke, Phys. Rev. Lett.122, 211801 (2019), arXiv:1812.08376 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  6. [6]

    Alekou et al

    A. Alekou et al. (ESSnuSB), Eur. Phys. J. ST 231, 3779 (2022), [Erratum: Eur.Phys.J.ST 232, 15–16 (2023)], arXiv:2206.01208 [hep-ex]

    work page arXiv 2022

  7. [7]

    Abeleet al., Phys

    H. Abeleet al., Phys. Rept.1023, 1 (2023), arXiv:2211.10396 [physics.ins-det]

    work page arXiv 2023

  8. [8]

    Alekouet al.(ESSnuSB), Universe9, 347 (2023), arXiv:2303.17356 [hep-ex]

    A. Alekouet al.(ESSnuSB), Universe9, 347 (2023), arXiv:2303.17356 [hep-ex]

    work page arXiv 2023

  9. [9]

    A Very Intense Neutrino Super Beam Experiment for Leptonic CP Violation Discovery based on the European Spallation Source Linac: A Snowmass 2013 White Paper

    E. Baussanet al.(ESSnuSB), Nucl. Phys. B885, 127 (2014), arXiv:1309.7022 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  10. [10]

    Exploring Source and Detector Non-Standard Neutrino Interactions at ESS$\nu$SB

    M. Blennow, S. Choubey, T. Ohlsson, and S. K. Raut, JHEP09, 096, arXiv:1507.02868 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  11. [11]

    L. A. Delgadillo and O. G. Miranda, Phys. Rev. D108, 095024 (2023), arXiv:2304.05545 [hep-ph]

    work page arXiv 2023

  12. [12]

    Aguilaret al.(ESSnuSB), Phys

    J. Aguilaret al.(ESSnuSB), Phys. Rev. D109, 115010 (2024), arXiv:2310.10749 [hep-ex]

    work page arXiv 2024

  13. [13]

    Baxteret al., JHEP02, 123, arXiv:1911.00762 [physics.ins-det]

    D. Baxteret al., JHEP02, 123, arXiv:1911.00762 [physics.ins-det]

    work page arXiv 1911

  14. [14]

    S. S. Chatterjee, S. Lavignac, O. G. Miranda, and G. Sanchez Garcia, Phys. Rev. D107, 055019 (2023), arXiv:2208.11771 [hep-ph]

    work page arXiv 2023

  15. [15]

    Simón (νESS), PoSTAUP2023, 171 (2024), arXiv:2401.04074 [hep-ex]

    A. Simón (νESS), PoSTAUP2023, 171 (2024), arXiv:2401.04074 [hep-ex]

    work page arXiv 2024

  16. [16]

    Ghosh, T

    M. Ghosh, T. Ohlsson, and S. Rosauro-Alcaraz, JHEP03, 026, arXiv:1912.10010 [hep-ph]

    work page arXiv 1912

  17. [17]

    Choubey, M

    S. Choubey, M. Ghosh, D. Kempe, and T. Ohlsson, JHEP05, 133, arXiv:2010.16334 [hep-ph]

    work page arXiv 2010

  18. [18]

    Majhi, D

    R. Majhi, D. K. Singha, K. N. Deepthi, and R. Mohanta, Phys. Rev. D104, 055002 (2021), arXiv:2101.08202 [hep-ph]

    work page arXiv 2021

  19. [19]

    S. S. Chatterjee, O. G. Miranda, M. Tórtola, and J. W. F. Valle, Phys. Rev. D106, 075016 (2022), arXiv:2111.08673 [hep-ph]

    work page arXiv 2022

  20. [20]

    Cordero, L

    R. Cordero, L. A. Delgadillo, and O. G. Miranda, Phys. Rev. D107, 075023 (2023), arXiv:2207.11308 [hep-ph]

    work page arXiv 2023

  21. [21]

    Cheng, M

    T. Cheng, M. Lindner, and W. Rodejohann, JHEP08, 111, arXiv:2204.10696 [hep-ph]

    work page arXiv

  22. [22]

    Aguilaret al.(ESSnuSB), JHEP08, 063, arXiv:2404.17559 [hep-ex]

    J. Aguilaret al.(ESSnuSB), JHEP08, 063, arXiv:2404.17559 [hep-ex]

    work page arXiv

  23. [23]

    Aguilaret al.(ESSnuSB), JHEP07, 186, arXiv:2504.10480 [hep-ph]

    J. Aguilaret al.(ESSnuSB), JHEP07, 186, arXiv:2504.10480 [hep-ph]

    work page arXiv

  24. [24]

    Aguilaret al.(ESSnuSB), JHEP10, 187, arXiv:2407.21663 [hep-ex]

    J. Aguilaret al.(ESSnuSB), JHEP10, 187, arXiv:2407.21663 [hep-ex]

    work page arXiv

  25. [25]

    The GENIE Neutrino Monte Carlo Generator

    C. Andreopouloset al.(GENIE), Nucl. Instrum. Meth. A614, 87 (2010), arXiv:0905.2517 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  26. [26]

    Alvarez-Rusoet al.(GENIE), Eur

    L. Alvarez-Rusoet al.(GENIE), Eur. Phys. J. ST230, 4449 (2021), arXiv:2106.09381 [hep-ph]

    work page arXiv 2021

  27. [27]

    Brun and F

    R. Brun and F. Rademakers, Nucl. Instrum. Meth. A389, 81 (1997)

    work page 1997

  28. [28]

    Simulation of long-baseline neutrino oscillation experiments with GLoBES

    P. Huber, M. Lindner, and W. Winter, Comput. Phys. Commun.167, 195 (2005), arXiv:hep-ph/0407333

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  29. [29]

    Huber, J

    P. Huber, J. Kopp, M. Lindner, M. Rolinec, and W. Winter, Comput. Phys. Commun.177, 432 (2007), arXiv:hep- ph/0701187

    work page arXiv 2007

  30. [30]

    J. Kopp, T. Ota, and W. Winter, Phys. Rev. D78, 053007 (2008), arXiv:0804.2261 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  31. [31]

    Blennow, E

    M. Blennow, E. Fernandez-Martinez, T. Ota, and S. Rosauro-Alcaraz, Eur. Phys. J. C80, 190 (2020), arXiv:1912.04309 [hep-ph]

    work page arXiv 2020

  32. [32]

    N. C. Ribeiro, H. Minakata, H. Nunokawa, S. Uchinami, and R. Zukanovich-Funchal, JHEP12, 002, arXiv:0709.1980 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 1980

  33. [33]

    Bounds on Non-Standard Neutrino Interactions Using PINGU

    S. Choubey and T. Ohlsson, Phys. Lett. B739, 357 (2014), arXiv:1410.0410 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  34. [34]

    Aielloet al.(KM3NeT), JCAP02, 073, arXiv:2411.19078 [hep-ex]

    S. Aielloet al.(KM3NeT), JCAP02, 073, arXiv:2411.19078 [hep-ex]

    work page arXiv

  35. [35]

    Abbasiet al.(IceCube), Phys

    R. Abbasiet al.(IceCube), Phys. Rev. Lett.129, 011804 (2022), arXiv:2201.03566 [hep-ex]

    work page arXiv 2022

  36. [36]

    Abbasiet al.(IceCube), Phys

    R. Abbasiet al.(IceCube), Phys. Rev. D104, 072006 (2021), arXiv:2106.07755 [hep-ex]

    work page arXiv 2021

  37. [37]

    Albertet al.(ANTARES), JHEP07, 048, arXiv:2112.14517 [hep-ex]

    A. Albertet al.(ANTARES), JHEP07, 048, arXiv:2112.14517 [hep-ex]

    work page arXiv

  38. [38]

    Study of Non-Standard Neutrino Interactions with Atmospheric Neutrino Data in Super-Kamiokande I and II

    G. Mitsukaet al.(Super-Kamiokande), Phys. Rev. D84, 113008 (2011), arXiv:1109.1889 [hep-ex]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  39. [39]

    Coloma, M.C

    P. Coloma, M. C. Gonzalez-Garcia, M. Maltoni, J. a. P. Pinheiro, and S. Urrea, JHEP08, 032, arXiv:2305.07698 [hep-ph]

    work page arXiv

  40. [40]

    A. M. Dziewonski and D. L. Anderson, Phys. Earth Planet. Interiors25, 297 (1981)

    work page 1981

  41. [41]

    Estebanet al.(NuFIT), Nufit 6.0,http://www.nu-fit.org/ (2024)

    I. Estebanet al.(NuFIT), Nufit 6.0,http://www.nu-fit.org/ (2024)

    work page 2024

  42. [42]

    Atmospheric neutrino flux calculation using the NRLMSISE00 atmospheric model

    M. Honda, M. Sajjad Athar, T. Kajita, K. Kasahara, and S. Midorikawa, Phys. Rev. D92, 023004 (2015), arXiv:1502.03916 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  43. [43]

    G. L. Fogli, E. Lisi, A. Marrone, D. Montanino, and A. Palazzo, Phys. Rev. D66, 053010 (2002), arXiv:hep-ph/0206162

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  44. [44]

    M. C. Gonzalez-Garcia and M. Maltoni, Phys. Rev. D70, 033010 (2004), arXiv:hep-ph/0404085

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  45. [45]

    Determining the Neutrino Mass Hierarchy with INO, T2K, NOvA and Reactor Experiments

    A. Ghosh, T. Thakore, and S. Choubey, JHEP04, 009, arXiv:1212.1305 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  46. [46]

    Constraints on the non-standard interaction in propagation from atmospheric neutrinos

    S. Fukasawa and O. Yasuda, Adv. High Energy Phys.2015, 820941 (2015), arXiv:1503.08056 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  47. [47]

    The possibility to observe the non-standard interaction by the Hyperkamiokande atmospheric neutrino experiment

    S. Fukasawa and O. Yasuda, Nucl. Phys. B914, 99 (2017), arXiv:1608.05897 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  48. [48]

    K. J. Kelly, Phys. Rev. D95, 115009 (2017), arXiv:1703.00448 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  49. [49]

    Neutrino Physics with Non-Standard Interactions at INO

    S. Choubey, A. Ghosh, T. Ohlsson, and D. Tiwari, JHEP12, 126, arXiv:1507.02211 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  50. [50]

    Atmospheric Neutrinos: Status and Prospects

    S. Choubey, Nucl. Phys. B908, 235 (2016), arXiv:1603.06841 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  51. [51]

    Neutrino Physics with JUNO

    F. Anet al.(JUNO), J. Phys. G43, 030401 (2016), arXiv:1507.05613 [physics.ins-det]. 14

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  52. [52]

    A., et al

    B. Abiet al.(DUNE), (2020), arXiv:2002.03005 [hep-ex]

    work page arXiv 2020

  53. [53]

    M. G. Aartsenet al.(IceCube-Gen2), J. Phys. G48, 060501 (2021), arXiv:2008.04323 [astro-ph.HE]

    work page arXiv 2021

  54. [54]

    Letter of Intent for KM3NeT 2.0

    S. Adrian-Martinezet al.(KM3Net), J. Phys. G43, 084001 (2016), arXiv:1601.07459 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  55. [55]

    Agostiniet al.(P-ONE), Nature Astron.4, 913 (2020), arXiv:2005.09493 [astro-ph.HE]

    M. Agostiniet al.(P-ONE), Nature Astron.4, 913 (2020), arXiv:2005.09493 [astro-ph.HE]

    work page arXiv 2020