Pith. sign in

REVIEW 4 major objections 5 minor 300 references

New Physics Opportunities at Neutrino Facilities: BSM Physics at Accelerator, Atmospheric, and Reactor Neutrino Experiments

T0 review · 4 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Neutrino facilities can double as a broad search machine for new physics, this white paper argues.

desk verdict A useful but under-edited workshop white paper that maps the BSM landscape at neutrino facilities; treat its sensitivity projections as design goals, not validated discovery potentials. read the letter →

arxiv 2506.15306 v2 pith:VCC33AN7 submitted 2025-06-18 hep-ph hep-ex

Koun Choi , Doojin Kim , Jong-Chul Park , Seodong Shin , Pouya Bakhti , Ki-Young Choi , Chang Hyon Ha , Kazumi Hata
show 17 more authors
Wooyoung Jang Yu Seon Jeong Young Ju Ko Hyun Su Lee Weijun Li Yu-Feng Li Mehedi Masud Kenny C. Y. Ng Jungsic Park Min-Gwa Park Komninos-John Plows Meshkat Rajaee Eunil Won Byeongsu Yang Seong Moon Yoo Jaehoon Yu Seokhoon Yun
This is my paper · ORCID
classification hep-phhep-ex
keywords darkmatteraxion-likeparticlesphotonssterileneutrinosnon-standardinteractionsneutrinofacilitiesbeamdumpexperimentsreactor
topics Dark Matter
open problems Dark Matter
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This white paper argues that the world's neutrino facilities, from accelerators and reactors to underground observatories, should be treated not only as tools for measuring neutrino oscillations but as a distributed machine for discovering physics beyond the Standard Model. It organizes the search landscape into laboratory-produced signals, such as dark photons, axion-like particles, light dark matter, sterile neutrinos, and non-standard interactions, and cosmogenic signals, such as boosted dark matter and neutrinos from dark-matter annihilation. The central claim is that the precision, timing, vertexing, and low-background capabilities being built for neutrino physics will reach unexplored parameter space for feebly interacting particles, often in regions connected to the dark-matter relic abundance and to anomalies like MiniBooNE, the reactor 5 MeV bump, and the Gallium deficit.

What carries the argument

The organizing mechanism is the two-channel classification of BSM signals by production origin: laboratory-produced signals from beam targets, dumps, and reactor cores, and cosmogenic signals from the atmosphere, the Sun, and astrophysical sources. The carrying technical instruments are the detector configurations that make those channels observable: short-baseline beam dumps with fine vertexing and sub-nanosecond timing (DAMSA), movable near detectors with flavor identification (DUNE-ND, IWCD), forward emulsion and liquid-argon detectors at the LHC (FASERnu, SND@LHC, FLArE), fixed-target hidden-sector spectrometers (SHiP), stopped-pion sources with pulsed timing (COHERENT, CCM, JSNS2), and large liquid-scintillator or water-Cherenkov observatories (JUNO, nu-EYE, Hyper-Kamiokande, IceCube-Gen2). These configurations supply the timing resolution, vertex precision, particle identification, and background suppression on which all the proposed searches rest.

What would settle it

A concrete test is to measure the beam-related neutron flux at the DAMSA target in the Stage 0 and Stage 3 validation runs; if the neutron-induced accidental diphoton rate exceeds the GEANT4 prediction by an order of magnitude at the proposed timing and vertex cuts, the DAMSA ALP sensitivity in the prompt-decay region would not hold. Likewise, a short-baseline reactor experiment with a gamma catcher such as RENE that fails to observe the predicted rate of the 3.685 MeV 13C de-excitation channel would undercut the proposed alternative probe of the 5 MeV bump.

Watch

Extended reading notes

Core claim

The paper claims that neutrino facilities offer substantial potential to search for new physics beyond neutrino oscillations, owing to their precision measurement capabilities, diverse experimental configurations, and multiple neutrino sources. It documents how accelerator-based experiments produce dark-sector particles through exotic meson decays and beam-target interactions, how reactors supply intense photon and antineutrino fluxes for axion and dark-photon searches, and how large underground detectors can catch cosmogenic boosted dark matter and annihilation neutrinos. For each channel, it reviews current limits from Super-Kamiokande, T2K, IceCube, JSNS2, NEOS, NEON, and KamLAND-Zen, then presents projected sensitivities for next-generation facilities including DAMSA, DUNE-ND, LHC forward detectors, SHiP, stopped-pion experiments, T2HK, IsoDAR@Yemilab, RENE, JUNO, Hyper-Kamiokande, and IceCube-Gen2. The paper concludes that these programs collectively probe new parameter space for dark matter, axion-like particles, dark photons, sterile neutrinos, and non-standard interactions, and it lists the detector capabilities and simulation tools required to realize those searches.

Load-bearing premise

The projected discovery reaches assume that next-generation detectors will actually achieve their specified background levels and efficiencies, for example that DAMSA's beam-related neutron background matches GEANT4 predictions pending its staged validation program, and that IsoDAR@Yemilab reaches a 2.26 kton fiducial volume with 92% inverse-beta-decay efficiency.

Editorial extensions

If this is right

  • If the projected sensitivities hold, a positive signal in any one channel, such as dark-matter-electron scattering at NEON or ALP decay to two photons at DAMSA, would be a discovery of physics beyond the Standard Model and could be cross-checked in the other listed facilities.
  • The combined program could cover light-mediator dark-matter parameter space consistent with the observed relic abundance, regions that direct-detection and collider experiments cannot currently reach.
  • Reactor-based detectors like JUNO-TAO and RENE would provide model-independent reference spectra that could resolve or sharpen the 5 MeV bump and the reactor antineutrino anomaly.
  • Forward detectors at the HL-LHC and SHiP would deliver first measurements of tau-neutrino and tau-antineutrino cross sections, enabling sterile-neutrino searches in the tau flavor.
  • Newly integrated simulation tools, such as GENIE-BDM and BeamHNL, would make BSM search projections reproducible and comparable across experiments.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the roadmap is correct, the global neutrino program effectively becomes an intensity-frontier dark-sector program, and a shared framework for background modeling and limit-setting across beam dumps, reactors, and observatories would accelerate cross-checks of any candidate signal.
  • The paper's emphasis on East Asian facilities suggests a geographic shift in neutrino science, with Yemilab, JUNO, and Hyper-Kamiokande collectively forming a regional hub for new-physics searches; the paper implicitly calls for stronger collaboration among these experiments.
  • The proposed 13C de-excitation channel to probe the 5 MeV bump is a testable extension: a dedicated measurement at RENE or IsoDAR could discriminate between nuclear-physics and beyond-the-Standard-Model explanations of the excess.
  • The sensitivity projections rely on simplified background assumptions in several cases, so a public comparison of projected versus achieved backgrounds after the first physics runs would calibrate the entire roadmap.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 5 minor

Summary. This paper is a review/white paper based on the 4th Workshop on New Physics Opportunities in Neutrino Facilities (NPN 2024). It organizes BSM searches at neutrino facilities into laboratory-produced and cosmogenic signals, summarizes recent experimental results from Super-Kamiokande, T2K, IceCube, JSNS2, NEOS, NEON, and KamLAND-Zen, and surveys projected sensitivities for a broad set of next-generation accelerator, reactor, and underground experiments, with particular emphasis on East Asian programs. The central claim is that neutrino facilities offer substantial potential to search for new physics beyond neutrino oscillations because of their precision, diverse configurations, and intense sources. The paper contains no new derivations; it compiles and interprets published studies and workshop presentations.

Significance. If taken as a roadmap, the paper is a useful and generally accurate survey of a rapidly growing field. Its strengths include up-to-date coverage of recent results such as the NEON light-dark-matter and ALP limits, explicit enumeration of detector capabilities needed for BSM searches, and concrete discussion of simulation tools (GENIE-BDM, BeamHNL) and staged validation plans. The qualitative central claim is already supported by current data, e.g., NEON's ALP and light-dark-matter limits and Super-Kamiokande and IceCube dark-matter searches, so it does not hinge on any single future projection. However, the quantitative parts of the roadmap rely heavily on projected sensitivities whose key assumptions are not yet demonstrated, several of them taken from studies by the workshop organizers themselves; the manuscript does not always clearly distinguish published results from preliminary projections. These weaknesses reduce the reliability of the quantitative claims but do not invalidate the broader thesis.

major comments (4)
  1. [IV.A.7] Section IV.A.7 contains large blocks of text and figures reproduced verbatim from Ref. [250] without clear quotation or attribution, including the repeated 'IBD analysis assumptions' table and figures using Ref. [250]'s internal numbering (its Fig. 4 and Fig. 5). The same blocks appear multiple times consecutively, making the section difficult to read. This must be rewritten with clear attribution, consistent figure and table numbering, and removal of duplicates before the paper can be evaluated for publication.
  2. [IV.A.1] The projected DAMSA ALP reach in Figs. 3 and 4 assumes suppression of beam-related-neutron (BRN) accidental diphoton backgrounds by about ten orders of magnitude, based on GEANT4 simulations. The manuscript's own staged plan lists proton-beam background validation as Stage 3, which has not yet been performed; only a 2 GeV mixed electron/pion beam test is reported. The text should state explicitly that the prompt-decay-region coverage is a projection contingent on Stage 3 validation, rather than presenting these contours as established experimental capabilities.
  3. [IV.A.7] The IsoDAR@Yemilab sensitivity shown in Fig. 10 depends on the assumptions in Table II: a 2.26 kton fiducial mass, 92% IBD efficiency, and 6.4%/sqrt(E) MeV energy resolution, for a slow-liquid-scintillator detector that has not yet demonstrated these properties. The sentence quoted from Ref. [250] that 'IsoDAR will almost certainly make a discovery' is an overclaim; the manuscript should frame this as a projected sensitivity under stated assumptions and explicitly note the dependence on unvalidated detector performance.
  4. [IV.A.1 and IV.A.7] Many of the quantitative projections in the roadmap are drawn from a small set of studies, several of which are authored by the workshop organizers (e.g., Refs. [73, 191, 192, 250]). This is not inherently inappropriate for a workshop summary, but the text should clearly label which sensitivity estimates are peer-reviewed results, which are preliminary projections, and which depend on detector performance that has not yet been demonstrated. Currently the narrative does not always make these distinctions.
minor comments (5)
  1. [II.A] There are several typos, including 'leptophilic intractions' (should be 'interactions'), 'sterline' (Section IV.A.2), 'udpated' (Section IV.A.3), 'readioactivity' (Section VI.A), 'preformed' (Section IV.A.2), and 'flor' (Section IV.A.7, should be 'fluor').
  2. [IV.A.7] The IsoDAR running time is given inconsistently: the text and Fig. 10 caption refer to both 4 years and 5 years of running for the 5 sigma sensitivity. These numbers should be reconciled.
  3. [IV.A.4] Reference [210] is incomplete, appearing only as '(2024).' with no title, authors, or journal information.
  4. [V.B] The phrase 'Atmospheric collider gives a robust and universal flux source of BSM search' is unclear and should be reworded, presumably to refer to cosmic-ray collisions in the atmosphere.
  5. [Fig. 12] The caption contains the typo 'Sesisitivity' instead of 'Sensitivity.'

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: this is a source-credited workshop review, and the quoted projections, including self-authored ones, are not derived from this paper's own inputs.

full rationale

The paper is a white-paper review based on workshop presentations, not a derivation. Its central claim that neutrino facilities offer substantial potential for BSM searches is qualitative and is independently supported by current experimental results summarized in Section III, including NEON's ALP and light-dark-matter limits, Super-Kamiokande dark-matter searches, and IceCube constraints. The future projections are quoted from external published studies with explicit source crediting, e.g., 'Plots taken from Ref. [191]', 'Plots taken from Ref. [192]', 'Table taken from Ref. [73]', and 'Plots taken from Ref. [250]'. No equation in this paper is equivalent by construction to an input, and no fitted parameter is renamed as a prediction. The DAMSA background-rejection claim is tied to a transparent staged validation plan, with Stage 3 ('Proton beam background validation') explicitly described as not yet performed; this is a stated limitation and a correctness risk, not a hidden circular step. Some cited projections originate from the same authors' earlier work, but the review's central case does not reduce to those citations, and self-citation alone is not circularity under the applicable rules. Accordingly, no significant circularity is present.

Assumptions & free parameters 3 free parameters · 3 assumptions · 0 invented entities

Because the paper is a review, it introduces no new free parameters or entities. The projections it presents rest on assumed detector performances and simulation fidelity from the cited works; I list the most load-bearing assumptions from the paper's own text.

free parameters (3)
  • IsoDAR@Yemilab fiducial mass = 2.26 kton
    Adopted from Refs. [73]/[250] for the sensitivity projections in Sec IV.A.7; a smaller realized mass would proportionally reduce event counts and weaken the exclusion reach.
  • Total IBD efficiency for IsoDAR@Yemilab = 92%
    Assumed in Table II; yields 1.67e6 detected IBD events over four years. Efficiency depends on analysis cuts and background rejection not yet demonstrated.
  • Background rate for nuEYE BDM search = about 1000 events per year (also 0-background case)
    Used in Fig. 14 to bracket sensitivity; real background rates depend on shielding and selection not yet implemented.
assumptions (3)
  • domain assumption GEANT4 simulations accurately predict beam-related neutron and photon backgrounds at short-baseline beam dumps.
    DAMSA feasibility (Sec IV.A.1) requires 10 orders of magnitude background suppression; Stage 0/3 validations are planned but not complete.
  • domain assumption Sensitivity projections reproduced from the cited papers are correct and assume realistic detector performance.
    The review's landscape relies on external projections (e.g., DUNE-ND sterile neutrino, SHiP, FPF, IsoDAR) without re-evaluating their assumptions.
  • domain assumption Standard Model neutrino fluxes and cross sections used in quoted projections are accurate.
    Signal and background estimates for reactor and accelerator searches depend on Huber-Mueller and other flux models, whose 5 MeV bump discrepancies are still unresolved (Sec II.A).

how reviews work

0 comments
Cite this review

Pith. "Pith review of New Physics Opportunities at Neutrino Facilities: BSM Physics at Accelerator, Atmospheric, and Reactor Neutrino Experiments." pith.science (2026). https://pith.science/paper/VCC33AN7

@misc{pith2026250615306,
  author       = {Pith},
  title        = {Pith review of: New Physics Opportunities at Neutrino Facilities: BSM Physics at Accelerator, Atmospheric, and Reactor Neutrino Experiments},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VCC33AN7}},
  note         = {Machine review of arXiv:2506.15306}
}
read the original abstract

Since the discovery of the Higgs boson, the long-standing task at hand in particle physics is the search for new physics beyond the Standard Model, which accounts for only about 5\% of the Universe. In light of this situation, the neutrino sector has drawn significant attention due to neutrino oscillations, which require physics beyond the Standard Model and have prompted a wide array of active and planned experimental programs. Notably, neutrino facilities offer substantial potential to search for new physics beyond neutrino oscillations, owing to their precision measurement capabilities, diverse experimental configurations, and various neutrino sources. This white paper summarizes the landscape of new physics that can be probed at current and future neutrino experiments, categorized into laboratory-produced and cosmogenic signals. We discuss recent experimental results interpreted through the lens of new physics, as well as detailed plans and projected sensitivities of next-generation facilities. This summary is based on presentations from the 4th Workshop on New Physics Opportunities in Neutrino Facilities (NPN 2024), held at IBS in Daejeon, Korea, on June 3-5, 2024. Particular emphasis is placed on accelerator-based neutrino experiments and a range of neutrino programs in East Asia. We also outline key tasks necessary to realize the promising new physics opportunities ahead.

Figures

Figures reproduced from arXiv: 2506.15306 by the authors.

Figure 1
Figure 1. FIG. 1. (a) The observed 90% C.L. exclusion limit (black solid line) on the light dark matter-electron [PITH_FULL_IMAGE:figures/full_fig_p013_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. A 3D model of a table=top scale DAMSA detector at the PIP-II proton beams [PITH_FULL_IMAGE:figures/full_fig_p016_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Left: 90% C.L. expected sensitivity reaches for the ALP-photon coupling parameter [PITH_FULL_IMAGE:figures/full_fig_p016_3.png] view at source ↗
Figures from the paper (12 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Top: 90% C.L. expected sensitivity estimates with the 300 MeV FAST electron beam at Fermilab for [PITH_FULL_IMAGE:figures/full_fig_p017_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p019_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. The projected exclusion limits on the dark matter model mediated by dark photon for two neutrino [PITH_FULL_IMAGE:figures/full_fig_p021_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Left: Expected constraints on mixing parameters for muon neutrinos in a presence of a sterile [PITH_FULL_IMAGE:figures/full_fig_p021_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. 90% C.L. projected experimental sensitivity to the vector-portal dark matter signals at COHERENT, [PITH_FULL_IMAGE:figures/full_fig_p024_8.png]
Figure 9
Figure 9. Figure 9: FIG. 9. The expected and actual 90% C.L. from CCM120 for the ALP-photon coupling [PITH_FULL_IMAGE:figures/full_fig_p025_9.png]
Figure 4
Figure 4. Figure 4: FIG. 4. The IsoDAR@Yemilab capability to measure oscillations under three example representative new physics scenarios: a with Kopp/Maltoni/Schwetz Parameters Dm2 = 1.35 eV2, sin22q = 0.214 and ! = 4.5 eV-1 6.4%/ pE (MeV) T (green) [57] and the combined [PITH_FULL_IMA…
Figure 10
Figure 10. Figure 10: FIG. 10. The IBD (¯⌫ [PITH_FULL_IMAGE:figures/full_fig_p028_10.png]
Figure 11
Figure 11. Figure 11: FIG. 11. Top: Example IBD event peaks from [PITH_FULL_IMAGE:figures/full_fig_p028_11.png]
Figure 12
Figure 12. Figure 12: FIG. 12. Sesisitivity estimates of the electron beam-dump program for Yemilab to [PITH_FULL_IMAGE:figures/full_fig_p029_12.png]
Figure 13
Figure 13. Figure 13: FIG. 13. The bottom panels of Fig. 8 of Ref. [ [PITH_FULL_IMAGE:figures/full_fig_p034_13.png]
Figure 14
Figure 14. Figure 14: FIG. 14. Top: The expected 90% C.L. sensitivities from 1-year and 5-year running of [PITH_FULL_IMAGE:figures/full_fig_p038_14.png]

Review history (2 revisions) →

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

300 extracted references · 15 canonical work pages

  1. [250]

    Artikovet al., Phys

    A. Artikovet al., Phys. Part. Nucl. Lett.19, 784 (2022)

    2022

  2. [1]

    Even with this limited dataset, NEON has already surpassed existing experimental limits in previously unexplored parameter regions

    NEON Upgrade Although NEON has collected physics data for nearly four years, the recent searches for beyond the Standard Model (BSM) physics, such as light dark matter [185] and ALPs [78], utilized only the initial 1.6 years of data. Even with this limited dataset, NEON has already surpassed existing experimental limits in previously unexplored parameter ...

  3. [2]

    The prototype detector consists of a cylindrical target with a Gd-loaded LS and a box-shaped gamma catcher filled with LS

    RENE Reactor Experiment for Neutrinos and Exotics (RENE), which is essentially the combined next generation program of NEOS and RENO, aims to probe sterile neutrino oscillation at ∆m2 41∼2 eV 2 region hinted by the joint analysis [251]. The prototype detector consists of a cylindrical target with a Gd-loaded LS and a box-shaped gamma catcher filled with L...

    2025

  4. [3]

    Eguchiet al.(KamLAND), Phys

    K. Eguchiet al.(KamLAND), Phys. Rev. Lett.90, 021802 (2003), arXiv:hep-ex/0212021

    arXiv 2003

  5. [4]

    It is designed to study neutrino properties with unprecedented precision, observe both astrophysical and terrestrial neutrinos, and search for new physics beyond the Standard Model

    JUNO & JUNO-TAO The Jiangmen Underground Neutrino Observatory (JUNO) is a multipurpose neutrino experi- ment located in Jiangmen, Kaiping, China [253, 254]. It is designed to study neutrino properties with unprecedented precision, observe both astrophysical and terrestrial neutrinos, and search for new physics beyond the Standard Model. The JUNO detector ...

    2024

  6. [5]

    The research and deconstruction work for KamLAND is currently underway [258]

    KamLAND2-Zen The KamLAND2-Zen is the next generation of the KamLAND-Zen experiment. The research and deconstruction work for KamLAND is currently underway [258]. The goal of KamLAND2- Zen experiment is the first search to cover the 3σband of the Majorana nature of neutrinos in the inverted mass ordering (IO) region. In order to achieved this goal, we need...

  7. [6]

    cosmic beam-dump

    AMoRE-II AMoRE-II aims to search for neutrinoless double beta decay of 100 kg of 100 Mo nuclei using molybdate scintillating crystals operating at milli-Kelvin temperatures. Currently, AMoRE-II is is under construction and will start data-taking at Yemilab in 2027. The muon veto system is now installed and its functionality is being tested [259]. The leve...

    2027

  8. [7]

    Fukudaet al.(Super-Kamiokande), Phys

    Y. Fukudaet al.(Super-Kamiokande), Phys. Rev. Lett.81, 1562 (1998), arXiv:hep-ex/9807003

    arXiv 1998

Show all 300 references
  1. [8]

    Q. R. Ahmadet al.(SNO), Phys. Rev. Lett.89, 011301 (2002), arXiv:nucl-ex/0204008

    2002 arXiv

  2. [9]

    A. A. Aguilar-Arevaloet al.(MiniBooNE), Phys. Rev. D103, 052002 (2021), arXiv:2006.16883 [hep- ex]

    2021 arXiv

  3. [10]

    M. H. Ahnet al.(K2K), Phys. Rev. Lett.90, 041801 (2003), arXiv:hep-ex/0212007

    2003 arXiv

  4. [11]

    C. A. Arg¨ uelleset al., Rept. Prog. Phys.83, 124201 (2020), arXiv:1907.08311 [hep-ph]

    2020 arXiv

  5. [12]

    Aguilar-Arevaloet al.(LSND), Phys

    A. Aguilar-Arevaloet al.(LSND), Phys. Rev. D64, 112007 (2001), arXiv:hep-ex/0104049

    2001 arXiv

  6. [13]

    A. A. Aguilar-Arevaloet al.(MiniBooNE), Phys. Rev. Lett.102, 101802 (2009), arXiv:0812.2243 [hep-ex]

    2009 arXiv

  7. [14]

    A. A. Aguilar-Arevaloet al.(MiniBooNE), Phys. Rev. Lett.121, 221801 (2018), arXiv:1805.12028 [hep-ex]

    2018 arXiv

  8. [15]

    S. G. Yoonet al.(RENO), Phys. Rev. D104, L111301 (2021), arXiv:2010.14989 [hep-ex]

    2021 arXiv

  9. [16]

    F. P. Anet al.(Daya Bay), Chin. Phys. C41, 013002 (2017), arXiv:1607.05378 [hep-ex]

    2017 arXiv

  10. [17]

    Y. J. Koet al.(NEOS), Phys. Rev. Lett.118, 121802 (2017), arXiv:1610.05134 [hep-ex]

    2017 arXiv

  11. [18]

    de Kerretet al.(Double Chooz), Nature Phys.16, 558 (2020), arXiv:1901.09445 [hep-ex]

    H. de Kerretet al.(Double Chooz), Nature Phys.16, 558 (2020), arXiv:1901.09445 [hep-ex]

    2020 arXiv

  12. [19]

    A. P. Serebrovet al., Phys. Rev. D104, 032003 (2021), arXiv:2005.05301 [hep-ex]

    2021 arXiv

  13. [20]

    Almaz´ anet al.(STEREO), J

    H. Almaz´ anet al.(STEREO), J. Phys. G48, 075107 (2021), arXiv:2010.01876 [hep-ex]

    2021 arXiv

  14. [21]

    precisely [91].νEYE may also be able to monitor reactor activities, by determining the distance and direction to reactor complexes via oscillation patterns and displacement vectors

  15. [22]

    Andriamiradoet al.(PROSPECT, (PROSPECT Collaboration)*), Phys

    M. Andriamiradoet al.(PROSPECT, (PROSPECT Collaboration)*), Phys. Rev. Lett.131, 021802 (2023), arXiv:2212.10669 [nucl-ex]

    2023 arXiv

  16. [23]

    Danilov (DANSS), Int

    M. Danilov (DANSS), Int. J. Mod. Phys. A39, 2443010 (2024)

    2024

  17. [24]

    T. A. Muelleret al., Phys. Rev. C83, 054615 (2011), arXiv:1101.2663 [hep-ex]

    2011 arXiv

  18. [25]

    Huber, Phys

    P. Huber, Phys. Rev. C84, 024617 (2011), [Erratum: Phys.Rev.C 85, 029901 (2012)], arXiv:1106.0687 [hep-ph]

    2011 arXiv

  19. [26]

    J. N. Abdurashitovet al., Phys. Rev. C73, 045805 (2006), arXiv:nucl-ex/0512041

    2006 arXiv

  20. [27]

    Hampelet al.(GALLEX), Phys

    W. Hampelet al.(GALLEX), Phys. Lett. B420, 114 (1998)

    1998

  21. [28]

    V. V. Barinovet al., Phys. Rev. Lett.128, 232501 (2022), arXiv:2109.11482 [nucl-ex]

    2022 arXiv

  22. [29]

    V. V. Barinovet al., Phys. Rev. C105, 065502 (2022), arXiv:2201.07364 [nucl-ex]

    2022 arXiv

  23. [30]

    Farzan, T

    Y. Farzan, T. Schwetz, and A. Y. Smirnov, JHEP07, 067 (2008), arXiv:0805.2098 [hep-ph]

    2008 arXiv

  24. [31]

    Bakhti, Y

    P. Bakhti, Y. Farzan, and T. Schwetz, JHEP05, 007 (2015), arXiv:1503.05374 [hep-ph]

    2015 arXiv

  25. [32]

    C. A. Arg¨ uelles, T. Bert´ olez-Mart´ ınez, and J. Salvado, Phys. Rev. D107, 036004 (2023), arXiv:2201.05108 [hep-ph]

    2023 arXiv

  26. [33]

    Hollenberg, O

    S. Hollenberg, O. Micu, and H. Pas, Phys. Rev. D80, 053010 (2009), arXiv:0906.5072 [hep-ph]

    2009 arXiv

  27. [34]

    Batellet al., inSnowmass 2021(2022) arXiv:2207.06898 [hep-ph]

    B. Batellet al., inSnowmass 2021(2022) arXiv:2207.06898 [hep-ph]

    2022 arXiv

  28. [35]

    Dentler, A

    M. Dentler, A. Hern´ andez-Cabezudo, J. Kopp, P. A. N. Machado, M. Maltoni, I. Martinez-Soler, and T. Schwetz, JHEP08, 010 (2018), arXiv:1803.10661 [hep-ph]

    2018 arXiv

  29. [36]

    Biggio, M

    C. Biggio, M. Blennow, and E. Fernandez-Martinez, JHEP08, 090 (2009), arXiv:0907.0097 [hep-ph]

    2009 arXiv

  30. [37]

    Bakhti, A

    P. Bakhti, A. N. Khan, and W. Wang, J. Phys. G44, 125001 (2017), arXiv:1607.00065 [hep-ph]

    2017 arXiv

  31. [38]

    M. C. Gonzalez-Garcia and M. Maltoni, JHEP09, 152 (2013), arXiv:1307.3092 [hep-ph]. 44

    2013 arXiv

  32. [39]

    Bakhti and Y

    P. Bakhti and Y. Farzan, JHEP07, 064 (2014), arXiv:1403.0744 [hep-ph]

    2014 arXiv

  33. [40]

    Coloma, M

    P. Coloma, M. C. Gonzalez-Garcia, M. Maltoni, and T. Schwetz, Phys. Rev. D96, 115007 (2017), arXiv:1708.02899 [hep-ph]

    2017 arXiv

  34. [41]

    Bakhti and Y

    P. Bakhti and Y. Farzan, JHEP07, 109 (2016), arXiv:1602.07099 [hep-ph]

    2016 arXiv

  35. [42]

    Bakhti and M

    P. Bakhti and M. Rajaee, Phys. Rev. D103, 075003 (2021), arXiv:2010.12849 [hep-ph]

    2021 arXiv

  36. [43]

    J. M. Berrymanet al., Phys. Dark Univ.42, 101267 (2023), arXiv:2203.01955 [hep-ph]

    2023 arXiv

  37. [44]

    Bakhti and Y

    P. Bakhti and Y. Farzan, Phys. Rev. D95, 095008 (2017), arXiv:1702.04187 [hep-ph]

    2017 arXiv

  38. [45]

    Bakhti, Y

    P. Bakhti, Y. Farzan, and M. Rajaee, Phys. Rev. D99, 055019 (2019), arXiv:1810.04441 [hep-ph]

    2019 arXiv

  39. [46]

    Bahraminasr, P

    M. Bahraminasr, P. Bakhti, and M. Rajaee, J. Phys. G48, 095001 (2021), arXiv:2003.09985 [hep-ph]

    2021 arXiv

  40. [47]

    Bakhti, M

    P. Bakhti, M. Rajaee, and S. Shin, Phys. Rev. D109, 095043 (2024), arXiv:2311.14945 [hep-ph]

    2024 arXiv

  41. [48]

    J. L. Fenget al., J. Phys. G50, 030501 (2023), arXiv:2203.05090 [hep-ex]

    2023 arXiv

  42. [49]

    P. S. B. Dev, D. Kim, D. Sathyan, K. Sinha, and Y. Zhang, (2024), arXiv:2407.12738 [hep-ph]

    2024 arXiv

  43. [50]

    R. Laha, B. Dasgupta, and J. F. Beacom, Phys. Rev. D89, 093025 (2014), arXiv:1304.3460 [hep-ph]

    2014 arXiv

  44. [51]

    Blennow, T

    M. Blennow, T. Ohlsson, and W. Winter, JHEP06, 049 (2005), arXiv:hep-ph/0502147

    2005 arXiv

  45. [52]

    Barger, C.-W

    V. Barger, C.-W. Chiang, W.-Y. Keung, and D. Marfatia, Phys. Rev. Lett.108, 081802 (2012), arXiv:1109.6652 [hep-ph]

    2012 arXiv

  46. [53]

    C. E. Carlson and B. C. Rislow, Phys. Rev. D86, 035013 (2012), arXiv:1206.3587 [hep-ph]

    2012 arXiv

  47. [54]

    Krnjaic, G

    G. Krnjaic, G. Marques-Tavares, D. Redigolo, and K. Tobioka, Phys. Rev. Lett.124, 041802 (2020), arXiv:1902.07715 [hep-ph]

    2020 arXiv

  48. [55]

    Dutta, D

    B. Dutta, D. Kim, A. Thompson, R. T. Thornton, and R. G. Van de Water, Phys. Rev. Lett.129, 111803 (2022), arXiv:2110.11944 [hep-ph]

    2022 arXiv

  49. [56]

    Dutta, A

    B. Dutta, A. Karthikeyan, D. Kim, A. Thompson, and R. G. Van de Water, (2025), arXiv:2504.08071 [hep-ph]

    2025 arXiv

  50. [57]

    A. A. Aguilar-Arevaloet al.(MiniBooNE DM), Phys. Rev. D98, 112004 (2018), arXiv:1807.06137 [hep-ex]

    2018 arXiv

  51. [58]

    Dutta, D

    B. Dutta, D. Kim, S. Liao, J.-C. Park, S. Shin, L. E. Strigari, and A. Thompson, JHEP01, 144 (2022), arXiv:2006.09386 [hep-ph]

    2022 arXiv

  52. [59]

    Celentano, L

    A. Celentano, L. Darm´ e, L. Marsicano, and E. Nardi, Phys. Rev. D102, 075026 (2020), arXiv:2006.09419 [hep-ph]

    2020 arXiv

  53. [60]

    A. A. Aguilar-Arevaloet al.(CCM), Phys. Rev. D109, 095017 (2024), [Addendum: Phys.Rev.D 111, 035030 (2025)], arXiv:2309.02599 [hep-ph]

    2024 arXiv

  54. [61]

    Agostinelliet al.(GEANT4), Nucl

    S. Agostinelliet al.(GEANT4), Nucl. Instrum. Meth. A506, 250 (2003)

    2003

  55. [62]

    Holdom, Phys

    B. Holdom, Phys. Lett. B166, 196 (1986)

    1986

  56. [63]

    L. B. Okun, Sov. Phys. JETP56, 502 (1982)

    1982

  57. [64]

    Patt and F

    B. Patt and F. Wilczek, (2006), arXiv:hep-ph/0605188

    2006 arXiv

  58. [65]

    Y. G. Kim, K. Y. Lee, and S. Shin, JHEP05, 100 (2008), arXiv:0803.2932 [hep-ph]

    2008 arXiv

  59. [66]

    Minkowski, Phys

    P. Minkowski, Phys. Lett. B67, 421 (1977)

    1977

  60. [67]

    R. D. Peccei and H. R. Quinn, Phys. Rev. Lett.38, 1440 (1977)

    1977

  61. [68]

    Weinberg, Phys

    S. Weinberg, Phys. Rev. Lett.40, 223 (1978)

    1978

  62. [69]

    Wilczek, Phys

    F. Wilczek, Phys. Rev. Lett.40, 279 (1978)

    1978

  63. [70]

    Svrcek and E

    P. Svrcek and E. Witten, JHEP06, 051 (2006), arXiv:hep-th/0605206

    2006 arXiv

  64. [71]

    W. M. Bonivento, D. Kim, and K. Sinha, Eur. Phys. J. C80, 164 (2020), arXiv:1909.03071 [hep-ph]

    2020 arXiv

  65. [72]

    J. B. Dent, B. Dutta, D. Kim, S. Liao, R. Mahapatra, K. Sinha, and A. Thompson, Phys. Rev. Lett. 124, 211804 (2020), arXiv:1912.05733 [hep-ph]

    2020 arXiv

  66. [73]

    Aristizabal Sierra, V

    D. Aristizabal Sierra, V. De Romeri, L. J. Flores, and D. K. Papoulias, JHEP03, 294 (2021), arXiv:2010.15712 [hep-ph]

    2021 arXiv

  67. [74]

    A. A. Aguilar-Arevaloet al.(CCM), Phys. Rev. D107, 095036 (2023), arXiv:2112.09979 [hep-ph]

    2023 arXiv

  68. [75]

    K. J. Kelly, S. Kumar, and Z. Liu, Phys. Rev. D103, 095002 (2021), arXiv:2011.05995 [hep-ph]. 45

    2021 arXiv

  69. [76]

    Brdar, B

    V. Brdar, B. Dutta, W. Jang, D. Kim, I. M. Shoemaker, Z. Tabrizi, A. Thompson, and J. Yu, Phys. Rev. Lett.126, 201801 (2021), arXiv:2011.07054 [hep-ph]

    2021 arXiv

  70. [77]

    Beachamet al., J

    J. Beachamet al., J. Phys. G47, 010501 (2020), arXiv:1901.09966 [hep-ex]

    2020 arXiv

  71. [78]

    Waites, A

    L. Waites, A. Thompson, A. Bungau, J. M. Conrad, B. Dutta, W.-C. Huang, D. Kim, M. Shaevitz, and J. Spitz, Phys. Rev. D107, 095010 (2023), arXiv:2207.13659 [hep-ph]

    2023 arXiv

  72. [79]

    Seoet al., (2023), arXiv:2309.13435 [hep-ex]

    S.-H. Seoet al., (2023), arXiv:2309.13435 [hep-ex]

    2023 arXiv

  73. [80]

    P. S. B. Dev, D. Kim, K. Sinha, and Y. Zhang, Phys. Rev. D104, 035037 (2021), arXiv:2101.08781 [hep-ph]

    2021 arXiv

  74. [81]

    Toupset al., inSnowmass 2021(2022) arXiv:2203.08079 [hep-ex]

    M. Toupset al., inSnowmass 2021(2022) arXiv:2203.08079 [hep-ex]

    2022 arXiv

  75. [82]

    Alekhinet al., Rept

    S. Alekhinet al., Rept. Prog. Phys.79, 124201 (2016), arXiv:1504.04855 [hep-ph]

    2016 arXiv

  76. [83]

    Albaneseet al.(SHiP),BDF/SHiP at the ECN3 high-intensity beam facility, Tech

    R. Albaneseet al.(SHiP),BDF/SHiP at the ECN3 high-intensity beam facility, Tech. Rep. (CERN, Geneva, 2023)

    2023

  77. [84]

    B. J. Parket al.(NEON), Phys. Rev. Lett.134, 201002 (2025), arXiv:2406.06117 [hep-ex]

    2025 arXiv

  78. [85]

    Mention, M

    G. Mention, M. Fechner, T. Lasserre, T. A. Mueller, D. Lhuillier, M. Cribier, and A. Letourneau, Phys. Rev. D83, 073006 (2011), arXiv:1101.2755 [hep-ex]

    2011 arXiv

  79. [86]

    Kopeikin, M

    V. Kopeikin, M. Skorokhvatov, and O. Titov, Phys. Rev. D104, L071301 (2021), arXiv:2103.01684 [nucl-ex]

    2021 arXiv

  80. [87]

    Estienneet al., Phys

    M. Estienneet al., Phys. Rev. Lett.123, 022502 (2019), arXiv:1904.09358 [nucl-ex]

    2019 arXiv

  81. [88]

    Danilov, PoSICHEP2022, 616 (2022), arXiv:2211.01208 [hep-ex]

    M. Danilov, PoSICHEP2022, 616 (2022), arXiv:2211.01208 [hep-ex]

    2022 arXiv

  82. [89]

    J. H. Choiet al.(RENO), Phys. Rev. Lett.116, 211801 (2016), arXiv:1511.05849 [hep-ex]

    2016 arXiv

  83. [90]

    F. P. Anet al.(Daya Bay), Phys. Rev. Lett.116, 061801 (2016), [Erratum: Phys.Rev.Lett. 118, 099902 (2017)], arXiv:1508.04233 [hep-ex]

    2016 arXiv

  84. [91]

    Abeet al.(Double Chooz), JHEP10, 086 (2014), [Erratum: JHEP 02, 074 (2015)], arXiv:1406.7763 [hep-ex]

    Y. Abeet al.(Double Chooz), JHEP10, 086 (2014), [Erratum: JHEP 02, 074 (2015)], arXiv:1406.7763 [hep-ex]

    2014 arXiv

  85. [92]

    Huber, Phys

    P. Huber, Phys. Rev. Lett.118, 042502 (2017), arXiv:1609.03910 [hep-ph]

    2017 arXiv

  86. [93]

    Hayen, J

    L. Hayen, J. Kostensalo, N. Severijns, and J. Suhonen, Phys. Rev. C100, 054323 (2019), arXiv:1908.08302 [nucl-th]

    2019 arXiv

  87. [94]

    J. M. Berryman, V. Brdar, and P. Huber, Phys. Rev. D99, 055045 (2019), arXiv:1803.08506 [hep-ph]

    2019 arXiv

  88. [95]

    Bakhti, M.-G

    P. Bakhti, M.-G. Park, M. Rajaee, C. S. Shin, and S. Shin, (2024), arXiv:2405.08724 [hep-ph]

    2024

  89. [96]

    Siyeon (NEOS), PoSICRC2017, 1024 (2018)

    K. Siyeon (NEOS), PoSICRC2017, 1024 (2018)

    2018

  90. [97]

    Bakhti, M

    P. Bakhti, M. Rajaee, S.-H. Seo, and S. Shin, Phys. Rev. D109, 095030 (2024), arXiv:2307.11582 [hep-ph]

    2024 arXiv

  91. [98]

    Bakhti and M

    P. Bakhti and M. Rajaee, Phys. Rev. D102, 035024 (2020), arXiv:2003.12984 [hep-ph]

    2020 arXiv

  92. [99]

    D’Eramo, G

    F. D’Eramo, G. Lucente, N. Nath, and S. Yun, JHEP12, 091 (2023), arXiv:2305.14420 [hep-ph]

    2023 arXiv

  93. [100]

    Maltoni and A

    M. Maltoni and A. Y. Smirnov, Eur. Phys. J. A52, 87 (2016), arXiv:1507.05287 [hep-ph]

    2016 arXiv

  94. [101]

    P. C. de Holanda and A. Y. Smirnov, Phys. Rev. D69, 113002 (2004), arXiv:hep-ph/0307266

    2004 arXiv

  95. [102]

    P. C. de Holanda and A. Y. Smirnov, Phys. Rev. D83, 113011 (2011), arXiv:1012.5627 [hep-ph]

    2011 arXiv

  96. [103]

    Bakhti and Y

    P. Bakhti and Y. Farzan, JHEP10, 200 (2013), arXiv:1308.2823 [hep-ph]

    2013 arXiv

  97. [104]

    Bakhti, M

    P. Bakhti, M. Rajaee, and S. Shin, Phys. Rev. D106, 115029 (2022), arXiv:2206.02594 [hep-ph]

    2022 arXiv

  98. [105]

    Weatherlyet al.(Super-Kamiokande), (2022), arXiv:2203.11772 [hep-ex]

    P. Weatherlyet al.(Super-Kamiokande), (2022), arXiv:2203.11772 [hep-ex]

    2022

  99. [106]

    Akita, S

    K. Akita, S. H. Im, M. Masud, and S. Yun, JHEP07, 057 (2024), arXiv:2312.13627 [hep-ph]

    2024 arXiv

  100. [107]

    C. A. Arg¨ uelles, A. Diaz, A. Kheirandish, A. Olivares-Del-Campo, I. Safa, and A. C. Vincent, Rev. Mod. Phys.93, 035007 (2021), arXiv:1912.09486 [hep-ph]

    2021 arXiv

  101. [108]

    L. S. Miranda, S. Basegmez du Pree, K. C. Y. Ng, A. Cheek, and C. Arina, JCAP08, 006 (2023), arXiv:2211.12235 [hep-ph]

    2023 arXiv

  102. [109]

    C. Rott, K. Kohri, and S. C. Park, Phys. Rev. D92, 023529 (2015), arXiv:1408.4575 [hep-ph]

    2015 arXiv

  103. [110]

    Abbasiet al.(IceCube), Phys

    R. Abbasiet al.(IceCube), Phys. Rev. D108, 102004 (2023), arXiv:2303.13663 [astro-ph.HE]

    2023

  104. [111]

    W. H. Press and D. N. Spergel, Astrophys. J.296, 679 (1985). 46

    1985

  105. [112]

    L. M. Krauss, K. Freese, W. Press, and D. Spergel, Astrophys. J.299, 1001 (1985)

    1985

  106. [113]

    M. G. Aartsenet al.(IceCube), (2017), arXiv:1710.01197 [astro-ph.HE]

    2017 arXiv

  107. [114]

    Abbasiet al.(IceCube), Phys

    R. Abbasiet al.(IceCube), Phys. Rev. D105, 062004 (2022), arXiv:2111.09970 [astro-ph.HE]

    2022

  108. [115]

    Kanget al.(IceCube), PoSICRC2023, 1380 (2023), arXiv:2308.02842 [astro-ph.HE]

    W. Kanget al.(IceCube), PoSICRC2023, 1380 (2023), arXiv:2308.02842 [astro-ph.HE]

    2023 arXiv

  109. [116]

    Desaiet al.(Super-Kamiokande), Phys

    S. Desaiet al.(Super-Kamiokande), Phys. Rev. D70, 083523 (2004), [Erratum: Phys.Rev.D 70, 109901 (2004)], arXiv:hep-ex/0404025

    2004 arXiv

  110. [117]

    Tanakaet al.(Super-Kamiokande), Astrophys

    T. Tanakaet al.(Super-Kamiokande), Astrophys. J.742, 78 (2011), arXiv:1108.3384 [astro-ph.HE]

    2011 arXiv

  111. [118]

    Choiet al.(Super-Kamiokande), Phys

    K. Choiet al.(Super-Kamiokande), Phys. Rev. Lett.114, 141301 (2015), arXiv:1503.04858 [hep-ex]

    2015 arXiv

  112. [119]

    Agashe, Y

    K. Agashe, Y. Cui, L. Necib, and J. Thaler, JCAP10, 062 (2014), arXiv:1405.7370 [hep-ph]

    2014 arXiv

  113. [120]

    Kim, J.-C

    D. Kim, J.-C. Park, and S. Shin, Phys. Rev. Lett.119, 161801 (2017), arXiv:1612.06867 [hep-ph]

    2017 arXiv

  114. [121]

    G. F. Giudice, D. Kim, J.-C. Park, and S. Shin, Phys. Lett. B780, 543 (2018), arXiv:1712.07126 [hep-ph]

    2018 arXiv

  115. [122]

    Bhattacharya, R

    A. Bhattacharya, R. Gandhi, and A. Gupta, JCAP03, 027 (2015), arXiv:1407.3280 [hep-ph]

    2015 arXiv

  116. [123]

    J. Kopp, J. Liu, and X.-P. Wang, JHEP04, 105 (2015), arXiv:1503.02669 [hep-ph]

    2015 arXiv

  117. [124]

    Heurtier, D

    L. Heurtier, D. Kim, J.-C. Park, and S. Shin, Phys. Rev. D100, 055004 (2019), arXiv:1905.13223 [hep-ph]

    2019 arXiv

  118. [125]

    Yin, EPJ Web Conf.208, 04003 (2019), arXiv:1809.08610 [hep-ph]

    W. Yin, EPJ Web Conf.208, 04003 (2019), arXiv:1809.08610 [hep-ph]

    2019 arXiv

  119. [126]

    Bringmann and M

    T. Bringmann and M. Pospelov, Phys. Rev. Lett.122, 171801 (2019), arXiv:1810.10543 [hep-ph]

    2019 arXiv

  120. [127]

    Y. Ema, F. Sala, and R. Sato, Phys. Rev. Lett.122, 181802 (2019), arXiv:1811.00520 [hep-ph]

    2019 arXiv

  121. [128]

    C. V. Cappiello, K. C. Y. Ng, and J. F. Beacom, Phys. Rev. D99, 063004 (2019), arXiv:1810.07705 [hep-ph]

    2019 arXiv

  122. [129]

    H. An, M. Pospelov, J. Pradler, and A. Ritz, Phys. Rev. Lett.120, 141801 (2018), [Erratum: Phys.Rev.Lett. 121, 259903 (2018)], arXiv:1708.03642 [hep-ph]

    2018 arXiv

  123. [130]

    Zhang, PTEP2022, 013B05 (2022), arXiv:2001.00948 [hep-ph]

    Y. Zhang, PTEP2022, 013B05 (2022), arXiv:2001.00948 [hep-ph]

    2022 arXiv

  124. [131]

    Jho, J.-C

    Y. Jho, J.-C. Park, S. C. Park, and P.-Y. Tseng, (2021), arXiv:2101.11262 [hep-ph]

    2021 arXiv

  125. [132]

    Das and M

    A. Das and M. Sen, Phys. Rev. D104, 075029 (2021), arXiv:2104.00027 [hep-ph]

    2021 arXiv

  126. [133]

    Lin, W.-H

    Y.-H. Lin, W.-H. Wu, M.-R. Wu, and H. T.-K. Wong, Phys. Rev. Lett.130, 111002 (2023), arXiv:2206.06864 [hep-ph]

    2023 arXiv

  127. [134]

    Lin and M.-R

    Y.-H. Lin and M.-R. Wu, Phys. Rev. Lett.133, 111004 (2024), arXiv:2404.08528 [hep-ph]

    2024 arXiv

  128. [135]

    J.-W. Wang, A. Granelli, and P. Ullio, Phys. Rev. Lett.128, 221104 (2022), arXiv:2111.13644 [astro- ph.HE]

    2022 arXiv

  129. [136]

    Alvey, M

    J. Alvey, M. Campos, M. Fairbairn, and T. You, Phys. Rev. Lett.123, 261802 (2019), arXiv:1905.05776 [hep-ph]

    2019 arXiv

  130. [137]

    C. A. Arg¨ uelles, V. Mu˜ noz, I. M. Shoemaker, and V. Takhistov, Phys. Lett. B833, 137363 (2022), arXiv:2203.12630 [hep-ph]

    2022 arXiv

  131. [138]

    DeRocco, P

    W. DeRocco, P. W. Graham, D. Kasen, G. Marques-Tavares, and S. Rajendran, Phys. Rev. D100, 075018 (2019), arXiv:1905.09284 [hep-ph]

    2019 arXiv

  132. [139]

    Calabrese, M

    R. Calabrese, M. Chianese, D. F. G. Fiorillo, and N. Saviano, Phys. Rev. D105, L021302 (2022), arXiv:2107.13001 [hep-ph]

    2022 arXiv

  133. [140]

    Kachuliset al.(Super-Kamiokande), Phys

    C. Kachuliset al.(Super-Kamiokande), Phys. Rev. Lett.120, 221301 (2018), arXiv:1711.05278 [hep- ex]

    2018 arXiv

  134. [141]

    Abeet al.(Super-Kamiokande), Phys

    K. Abeet al.(Super-Kamiokande), Phys. Rev. Lett.130, 031802 (2023), [Erratum: Phys.Rev.Lett. 131, 159903 (2023)], arXiv:2209.14968 [hep-ex]

    2023 arXiv

  135. [142]

    Haet al.(COSINE-100), Phys

    C. Haet al.(COSINE-100), Phys. Rev. Lett.122, 131802 (2019), arXiv:1811.09344 [astro-ph.IM]

    2019 arXiv

  136. [143]

    Adhikariet al.(COSINE-100), Phys

    G. Adhikariet al.(COSINE-100), Phys. Rev. Lett.131, 201802 (2023), arXiv:2306.00322 [hep-ex]

    2023 arXiv

  137. [144]

    Cuiet al.(PandaX-II), Phys

    X. Cuiet al.(PandaX-II), Phys. Rev. Lett.128, 171801 (2022), arXiv:2112.08957 [hep-ex]

    2022 arXiv

  138. [145]

    Shanget al.(PandaX), Phys

    X. Shanget al.(PandaX), Phys. Rev. Lett.133, 101805 (2024), arXiv:2403.08361 [hep-ex]

    2024 arXiv

  139. [146]

    Xuet al.(CDEX), Phys

    R. Xuet al.(CDEX), Phys. Rev. D106, 052008 (2022), arXiv:2201.01704 [hep-ex]. 47

    2022 arXiv

  140. [147]

    Z. H. Zhanget al.(CDEX), Phys. Rev. D108, 052006 (2023), arXiv:2211.07477 [hep-ex]

    2023 arXiv

  141. [148]

    N. Y. Agafonovaet al.(NEWSdm), JCAP07, 067 (2023), arXiv:2305.00112 [astro-ph.IM]

    2023 arXiv

  142. [149]

    Aalberset al.(LZ), (2025), arXiv:2503.18158 [hep-ex]

    J. Aalberset al.(LZ), (2025), arXiv:2503.18158 [hep-ex]

    2025 arXiv

  143. [150]

    Agneset al.(DarkSide-50), (2025), arXiv:2505.13093 [hep-ph]

    P. Agneset al.(DarkSide-50), (2025), arXiv:2505.13093 [hep-ph]

    2025

  144. [151]

    Abiet al.(DUNE), Eur

    B. Abiet al.(DUNE), Eur. Phys. J. C81, 322 (2021), arXiv:2008.12769 [hep-ex]

    2021

  145. [152]

    De Roeck, D

    A. De Roeck, D. Kim, Z. G. Moghaddam, J.-C. Park, S. Shin, and L. H. Whitehead, JHEP11, 043 (2020), arXiv:2005.08979 [hep-ph]

    2020 arXiv

  146. [153]

    D. Kim, P. A. N. Machado, J.-C. Park, and S. Shin, JHEP07, 057 (2020), arXiv:2003.07369 [hep-ph]

    2020 arXiv

  147. [154]

    Choi and J.-C

    K. Choi and J.-C. Park, (2024), arXiv:2409.05646 [hep-ph]

    2024 arXiv

  148. [155]

    D. Kim, K. Kong, J.-C. Park, and S. Shin, JHEP08, 155 (2018), arXiv:1804.07302 [hep-ph]

    2018 arXiv

  149. [156]

    Chatterjee, A

    A. Chatterjee, A. De Roeck, D. Kim, Z. G. Moghaddam, J.-C. Park, S. Shin, L. H. Whitehead, and J. Yu, Phys. Rev. D98, 075027 (2018), arXiv:1803.03264 [hep-ph]

    2018 arXiv

  150. [157]

    Coloma, J

    P. Coloma, J. L´ opez-Pav´ on, L. Molina-Bueno, and S. Urrea, JHEP01, 134 (2024), arXiv:2304.06765 [hep-ph]

    2024 arXiv

  151. [158]

    Guo, Y.-L

    G. Guo, Y.-L. S. Tsai, and M.-R. Wu, JCAP10, 049 (2020), arXiv:2004.03161 [astro-ph.HE]

    2020 arXiv

  152. [159]

    C. V. Cappiello, Q. Liu, G. Mohlabeng, and A. C. Vincent, Phys. Rev. D110, 095031 (2024), arXiv:2405.00086 [hep-ph]

    2024 arXiv

  153. [160]

    Plestid, V

    R. Plestid, V. Takhistov, Y.-D. Tsai, T. Bringmann, A. Kusenko, and M. Pospelov, Phys. Rev. D 102, 115032 (2020), arXiv:2002.11732 [hep-ph]

    2020 arXiv

  154. [161]

    Coloma, P

    P. Coloma, P. Hern´ andez, V. Mu˜ noz, and I. M. Shoemaker, Eur. Phys. J. C80, 235 (2020), arXiv:1911.09129 [hep-ph]

    2020 arXiv

  155. [162]

    Atkinson, P

    M. Atkinson, P. Coloma, I. Martinez-Soler, N. Rocco, and I. M. Shoemaker, JHEP04, 174 (2022), arXiv:2105.09357 [hep-ph]

    2022 arXiv

  156. [163]

    Book Motzkin, PoST AUP2023, 338 (2024)

    J. Book Motzkin, PoST AUP2023, 338 (2024)

    2024

  157. [164]

    Iguro, R

    S. Iguro, R. Plestid, and V. Takhistov, Phys. Rev. Lett.128, 201101 (2022), arXiv:2111.12091 [hep- ph]

    2022 arXiv

  158. [165]

    Abbasiet al.(ICECUBE, IceCube), Nature Phys.20, 913 (2024), arXiv:2308.00105 [hep-ex]

    R. Abbasiet al.(ICECUBE, IceCube), Nature Phys.20, 913 (2024), arXiv:2308.00105 [hep-ex]

    2024

  159. [166]

    Mitsukaet al.(Super-Kamiokande), Phys

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

    2011 arXiv

  160. [167]

    Taani,Non-Standard Neutrino Interaction Analysis with Atmospheric Neutrino Data in Super- Kamiokande I-IV and the Design of the Hyper-Kamiokande Outer Detector, Ph.D

    M. Taani,Non-Standard Neutrino Interaction Analysis with Atmospheric Neutrino Data in Super- Kamiokande I-IV and the Design of the Hyper-Kamiokande Outer Detector, Ph.D. thesis, Nagoya University/The University of Edinburgh, Edinburgh U. (2020)

    2020

  161. [168]

    Abeet al.(Super-Kamiokande), Phys

    K. Abeet al.(Super-Kamiokande), Phys. Rev. D91, 052003 (2015), arXiv:1410.4267 [hep-ex]

    2015 arXiv

  162. [169]

    Abeet al.(Super-Kamiokande), Phys

    K. Abeet al.(Super-Kamiokande), Phys. Rev. D91, 052019 (2015), arXiv:1410.2008 [hep-ex]

    2015 arXiv

  163. [170]

    Mijakowski (Super-Kamiokande), J

    P. Mijakowski (Super-Kamiokande), J. Phys. Conf. Ser.718, 042040 (2016)

    2016

  164. [171]

    Frankiewicz (Super-Kamiokande), inMeeting of the APS Division of Particles and Fields(2015) arXiv:1510.07999 [hep-ex]

    K. Frankiewicz (Super-Kamiokande), inMeeting of the APS Division of Particles and Fields(2015) arXiv:1510.07999 [hep-ex]

    2015 arXiv

  165. [172]

    Abeet al.(T2K), Nucl

    K. Abeet al.(T2K), Nucl. Instrum. Meth. A659, 106 (2011), arXiv:1106.1238 [physics.ins-det]

    2011

  166. [173]

    Abeet al.(T2K), Phys

    K. Abeet al.(T2K), Phys. Rev. D100, 052006 (2019), arXiv:1902.07598 [hep-ex]

    2019 arXiv

  167. [174]

    S. S. Chatterjee and A. Palazzo, Phys. Rev. Lett.126, 051802 (2021), arXiv:2008.04161 [hep-ph]

    2021 arXiv

  168. [175]

    Majhi, D

    R. Majhi, D. K. Singha, K. N. Deepthi, and R. Mohanta, Eur. Phys. J. C82, 919 (2022), arXiv:2205.04269 [hep-ph]

    2022 arXiv

  169. [176]

    L. S. Miranda, P. Pasquini, U. Rahaman, and S. Razzaque, Eur. Phys. J. C81, 444 (2021), arXiv:1911.09398 [hep-ph]

    2021 arXiv

  170. [177]

    S. S. Chatterjee and A. Palazzo, (2020), arXiv:2005.10338 [hep-ph]

    2020 arXiv

  171. [178]

    de Gouvˆ ea, G

    A. de Gouvˆ ea, G. Jusino S´ anchez, and K. J. Kelly, Phys. Rev. D106, 055025 (2022), arXiv:2204.09130 [hep-ph]

    2022 arXiv

  172. [179]

    H.-X. Lin, J. Tang, and S. Vihonen, (2023), arXiv:2312.11704 [hep-ph]. 48

    2023 arXiv

  173. [180]

    M. G. Aartsenet al.(IceCube), JINST12, P03012 (2017), [Erratum: JINST 19, E05001 (2024)], arXiv:1612.05093 [astro-ph.IM]

    2017 arXiv

  174. [181]

    Abbasiet al.(IceCube), Science380, adc9818 (2023), arXiv:2307.04427 [astro-ph.HE]

    R. Abbasiet al.(IceCube), Science380, adc9818 (2023), arXiv:2307.04427 [astro-ph.HE]

    2023

  175. [182]

    R. Naab, E. Ganster, and Z. Zhang (IceCube), in38th International Cosmic Ray Conference(2023) arXiv:2308.00191 [astro-ph.HE]

    2023 arXiv

  176. [183]

    Abbasiet al.(IceCube), Science378, 538 (2022), arXiv:2211.09972 [astro-ph.HE]

    R. Abbasiet al.(IceCube), Science378, 538 (2022), arXiv:2211.09972 [astro-ph.HE]

    2022

  177. [184]

    Ageronet al.(KM3NeT, ANTARES), PoSICRC2021, 537 (2021)

    M. Ageronet al.(KM3NeT, ANTARES), PoSICRC2021, 537 (2021)

    2021

  178. [185]

    Abbasiet al.(IceCube), PoSICRC2021, 020 (2022)

    R. Abbasiet al.(IceCube), PoSICRC2021, 020 (2022)

    2022

  179. [186]

    Renzi and J

    G. Renzi and J. A. Aguilar (IceCube), in38th International Cosmic Ray Conference(2023) arXiv:2308.02920 [astro-ph.HE]

    2023 arXiv

  180. [187]

    Abbasiet al.(IceCube), PoSICRC2023, 1378 (2023), arXiv:2308.04833 [astro-ph.HE]

    R. Abbasiet al.(IceCube), PoSICRC2023, 1378 (2023), arXiv:2308.04833 [astro-ph.HE]

    2023 arXiv

  181. [188]

    Hinoet al.(JSNS2), Eur

    Y. Hinoet al.(JSNS2), Eur. Phys. J. C82, 331 (2022), arXiv:2111.07482 [hep-ex]

    2022 arXiv

  182. [189]

    D. H. Leeet al.(JSNS2), Eur. Phys. J. C84, 409 (2024), arXiv:2308.02722 [hep-ex]

    2024 arXiv

  183. [190]

    Y. J. Koet al.(NEOS Collaboration), Phys. Rev. Lett.118, 121802 (2017)

    2017

  184. [191]

    J. J. Choiet al.(NEON), Phys. Rev. Lett.134, 021802 (2025), arXiv:2407.16194 [hep-ex]

    2025 arXiv

  185. [192]

    J. J. Choiet al.(NEON), Eur. Phys. J. C83, 226 (2023), arXiv:2204.06318 [hep-ex]

    2023 arXiv

  186. [193]

    J. J. Choiet al.(NEON), JINST19, P10020 (2024), arXiv:2404.03691 [physics.ins-det]

    2024 arXiv

  187. [194]

    Abeet al.(KamLAND-Zen), (2024), arXiv:2406.11438 [hep-ex]

    S. Abeet al.(KamLAND-Zen), (2024), arXiv:2406.11438 [hep-ex]

    2024

  188. [195]

    Gandoet al.(KamLAND-Zen), Phys

    A. Gandoet al.(KamLAND-Zen), Phys. Rev. C86, 021601(R) (2012), arXiv:1205.6372 [hep-ex]

    2012 arXiv

  189. [196]

    Abeet al.(KamLAND-Zen), Phys

    S. Abeet al.(KamLAND-Zen), Phys. Lett. B855, 138846 (2024), arXiv:2311.09676 [hep-ex]

    2024

  190. [197]

    W. Jang, D. Kim, K. Kong, Y. Kwon, J.-C. Park, M. S. Ryu, S. Shin, R. G. Van de Water, U.-K. Yang, and J. Yu, Phys. Rev. D107, L031901 (2023), arXiv:2207.02223 [hep-ph]

    2023 arXiv

  191. [198]

    D. Kim, J. Yu, J.-C. Park, and H. Kim, (2024), arXiv:2401.09529 [hep-ph]

    2024 arXiv

  192. [199]

    Abiet al.(DUNE), JINST15, T08008 (2020), arXiv:2002.02967 [physics.ins-det]

    B. Abiet al.(DUNE), JINST15, T08008 (2020), arXiv:2002.02967 [physics.ins-det]. [194]SURF,https://sanfordlab.org/

    2020

  193. [200]

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

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

    2020

  194. [201]

    Abiet al.(DUNE), (2021), arXiv:2103.04797 [hep-ex]

    B. Abiet al.(DUNE), (2021), arXiv:2103.04797 [hep-ex]

    2021

  195. [202]

    Gandhi, B

    R. Gandhi, B. Kayser, M. Masud, and S. Prakash, JHEP11, 039 (2015), arXiv:1508.06275 [hep-ph]

    2015 arXiv

  196. [203]

    Dutta, R

    D. Dutta, R. Gandhi, B. Kayser, M. Masud, and S. Prakash, JHEP11, 122 (2016), arXiv:1607.02152 [hep-ph]

    2016 arXiv

  197. [204]

    Huber, M

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

    2005

  198. [205]

    Huber, J

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

    2007 arXiv

  199. [206]

    Parveen, M

    S. Parveen, M. Masud, M. Bishai, and P. Mehta, JHEP01, 139 (2025), arXiv:2409.17878 [hep-ph]

    2025 arXiv

  200. [207]

    Adamsonet al.(Daya Bay, MINOS), Phys

    P. Adamsonet al.(Daya Bay, MINOS), Phys. Rev. Lett.117, 151801 (2016), [Addendum: Phys.Rev.Lett. 117, 209901 (2016)], arXiv:1607.01177 [hep-ex]

    2016 arXiv

  201. [208]

    Adamsonet al.(MINOS+), Phys

    P. Adamsonet al.(MINOS+), Phys. Rev. Lett.122, 091803 (2019), arXiv:1710.06488 [hep-ex]

    2019 arXiv

  202. [209]

    Ahdidaet al.(SHiP), (2020), arXiv:2002.08722 [physics.ins-det]

    C. Ahdidaet al.(SHiP), (2020), arXiv:2002.08722 [physics.ins-det]

    2020

  203. [210]

    Acamporaet al.(SND@LHC), JINST19, P05067 (2024), arXiv:2210.02784 [hep-ex]

    G. Acamporaet al.(SND@LHC), JINST19, P05067 (2024), arXiv:2210.02784 [hep-ex]

    2024 arXiv

  204. [211]

    Arigaet al.(FASER), (2018), arXiv:1812.09139 [physics.ins-det]

    A. Arigaet al.(FASER), (2018), arXiv:1812.09139 [physics.ins-det]

    2018 arXiv

  205. [212]

    Arigaet al.(FASER), (2019), arXiv:1901.04468 [hep-ex]

    A. Arigaet al.(FASER), (2019), arXiv:1901.04468 [hep-ex]

    2019 arXiv

  206. [213]

    Abreuet al.(FASER), (2020), arXiv:2001.03073 [physics.ins-det]

    H. Abreuet al.(FASER), (2020), arXiv:2001.03073 [physics.ins-det]

    2020 arXiv

  207. [214]

    L. A. Anchordoquiet al., Phys. Rept.968, 1 (2022), arXiv:2109.10905 [hep-ph]

    2022 arXiv

  208. [215]

    Batell, J

    B. Batell, J. L. Feng, A. Ismail, F. Kling, R. M. Abraham, and S. Trojanowski, Phys. Rev. D104, 035036 (2021), arXiv:2107.00666 [hep-ph]. 49

    2021 arXiv

  209. [216]

    Batell, J

    B. Batell, J. L. Feng, and S. Trojanowski, Phys. Rev. D103, 075023 (2021), arXiv:2101.10338 [hep- ph]

    2021 arXiv

  210. [217]

    J. P. Leeset al.(BaBar), Phys. Rev. Lett.119, 131804 (2017), arXiv:1702.03327 [hep-ex]

    2017 arXiv

  211. [218]

    Grassleret al.(BEBC WA66), Nucl

    H. Grassleret al.(BEBC WA66), Nucl. Phys. B273, 253 (1986)

    1986

  212. [219]

    B. Wang, J. Bian, T. E. Coan, S. Kotelnikov, H. Duyang, and A. Hatzikoutelis (NOvA), J. Phys. Conf. Ser.888, 012123 (2017)

    2017

  213. [220]

    Batell, R

    B. Batell, R. Essig, and Z. Surujon, Phys. Rev. Lett.113, 171802 (2014), arXiv:1406.2698 [hep-ph]

    2014 arXiv

  214. [221]

    Banerjeeet al., Phys

    D. Banerjeeet al., Phys. Rev. Lett.123, 121801 (2019), arXiv:1906.00176 [hep-ex]

    2019 arXiv

  215. [222]

    deNiverville, M

    P. deNiverville, M. Pospelov, and A. Ritz, Phys. Rev. D84, 075020 (2011), arXiv:1107.4580 [hep-ph]

    2011 arXiv

  216. [223]

    Altmannshoferet al.(Belle-II), PTEP2019, 123C01 (2019), [Erratum: PTEP 2020, 029201 (2020)], arXiv:1808.10567 [hep-ex]

    W. Altmannshoferet al.(Belle-II), PTEP2019, 123C01 (2019), [Erratum: PTEP 2020, 029201 (2020)], arXiv:1808.10567 [hep-ex]

    2019

  217. [224]

    ˚Akessonet al.(LDMX), (2018), arXiv:1808.05219 [hep-ex]

    T. ˚Akessonet al.(LDMX), (2018), arXiv:1808.05219 [hep-ex]

    2018 arXiv

  218. [225]

    S. N. Gninenko, D. V. Kirpichnikov, M. M. Kirsanov, and N. V. Krasnikov, Phys. Lett. B796, 117 (2019), arXiv:1903.07899 [hep-ph]

    2019 arXiv

  219. [226]

    Ahdidaet al.(SHiP), JHEP04, 199 (2021), arXiv:2010.11057 [hep-ex]

    C. Ahdidaet al.(SHiP), JHEP04, 199 (2021), arXiv:2010.11057 [hep-ex]

    2021 arXiv

  220. [227]

    Battaglieriet al.(BDX), (2016), arXiv:1607.01390 [hep-ex]

    M. Battaglieriet al.(BDX), (2016), arXiv:1607.01390 [hep-ex]

    2016 arXiv

  221. [228]

    Batell, J

    B. Batell, J. L. Feng, M. Fieg, A. Ismail, F. Kling, R. M. Abraham, and S. Trojanowski, Phys. Rev. D105, 075001 (2022), arXiv:2111.10343 [hep-ph]

    2022 arXiv

  222. [229]

    Boyarsky, O

    A. Boyarsky, O. Mikulenko, M. Ovchynnikov, and L. Shchutska, JHEP03, 006 (2022), arXiv:2104.09688 [hep-ph]

    2022 arXiv

  223. [230]

    W. Bai, M. Diwan, M. V. Garzelli, Y. S. Jeong, and M. H. Reno, JHEP06, 032 (2020), arXiv:2002.03012 [hep-ph]

    2020 arXiv

  224. [231]

    K.-Y. Choi, S. H. Kim, Y. G. Kim, K. Y. Lee, K. S. Lee, B. D. Park, J. Y. Sohn, S. M. Yoo, and C. S. Yoon, JHEP06, 166 (2024), [Erratum: JHEP Grav.Cosmol. 01, 36 (2025)], arXiv:2403.04191 [hep-ph]

    2024 arXiv

  225. [232]

    K.-Y. Choi, Y. S. Jeong, S. H. Kim, Y. G. Kim, K. Y. Lee, K. S. Lee, B. D. Park, J. Y. Sohn, S. M. Yoo, and C. S. Yoon, (2025), arXiv:2505.12785 [hep-ph]

    2025 arXiv

  226. [233]

    Magill, R

    G. Magill, R. Plestid, M. Pospelov, and Y.-D. Tsai, Phys. Rev. Lett.122, 071801 (2019), arXiv:1806.03310 [hep-ph]

    2019 arXiv

  227. [234]

    Ovchynnikov, J.-L

    M. Ovchynnikov, J.-L. Tastet, O. Mikulenko, and K. Bondarenko, Phys. Rev. D108, 075028 (2023), arXiv:2305.13383 [hep-ph]

    2023 arXiv

  228. [235]

    Ajimuraet al.(JSNS2), (2020), arXiv:2012.10807 [hep-ex]

    S. Ajimuraet al.(JSNS2), (2020), arXiv:2012.10807 [hep-ex]

    2020 arXiv

  229. [236]

    deNiverville, M

    P. deNiverville, M. Pospelov, and A. Ritz, Phys. Rev. D92, 095005 (2015), arXiv:1505.07805 [hep-ph]

    2015 arXiv

  230. [237]

    Ge and I

    S.-F. Ge and I. M. Shoemaker, JHEP11, 066 (2018), arXiv:1710.10889 [hep-ph]

    2018 arXiv

  231. [238]

    Berlin, P

    A. Berlin, P. deNiverville, A. Ritz, P. Schuster, and N. Toro, Phys. Rev. D102, 095011 (2020), arXiv:2003.03379 [hep-ph]

    2020 arXiv

  232. [239]

    Dutta, D

    B. Dutta, D. Kim, S. Liao, J.-C. Park, S. Shin, and L. E. Strigari, Phys. Rev. Lett.124, 121802 (2020), arXiv:1906.10745 [hep-ph]

    2020 arXiv

  233. [240]

    Akimovet al.(COHERENT), Phys

    D. Akimovet al.(COHERENT), Phys. Rev. D102, 052007 (2020), arXiv:1911.06422 [hep-ex]

    2020 arXiv

  234. [241]

    A. A. Aguilar-Arevaloet al., (2023), arXiv:2311.09915 [hep-ex]

    2023 arXiv

  235. [242]

    Abeet al.(T2K), (2019), arXiv:1901.03750 [physics.ins-det]

    K. Abeet al.(T2K), (2019), arXiv:1901.03750 [physics.ins-det]

    2019

  236. [243]

    Korzenevet al., JINST17, P01016 (2022), arXiv:2109.03078 [physics.ins-det]

    A. Korzenevet al., JINST17, P01016 (2022), arXiv:2109.03078 [physics.ins-det]

    2022 arXiv

  237. [244]

    Atti´ eet al., Nucl

    D. Atti´ eet al., Nucl. Instrum. Meth. A957, 163286 (2020), arXiv:1907.07060 [physics.ins-det]

    2020 arXiv

  238. [245]

    Atti´ eet al., Nucl

    D. Atti´ eet al., Nucl. Instrum. Meth. A1025, 166109 (2022), arXiv:2106.12634 [physics.ins-det]

    2022 arXiv

  239. [246]

    Blondelet al., JINST15, P12003 (2020), arXiv:2008.08861 [physics.ins-det]

    A. Blondelet al., JINST15, P12003 (2020), arXiv:2008.08861 [physics.ins-det]

    2020 arXiv

  240. [247]

    Agarwalet al., Phys

    A. Agarwalet al., Phys. Lett. B840, 137843 (2023), arXiv:2207.02685 [physics.ins-det]

    2023 arXiv

  241. [248]

    deNiverville, C.-Y

    P. deNiverville, C.-Y. Chen, M. Pospelov, and A. Ritz, Phys. Rev. D95, 035006 (2017), arXiv:1609.01770 [hep-ph]. 50

    2017 arXiv

  242. [249]

    Araki, K

    T. Araki, K. Asai, T. Iizawa, H. Otono, T. Shimomura, and Y. Takubo, JHEP11, 056 (2023), arXiv:2308.01565 [hep-ph]

    2023 arXiv

  243. [251]

    Gorbunov, I

    D. Gorbunov, I. Krasnov, Y. Kudenko, and S. Suvorov, Phys. Lett. B822, 136641 (2021), arXiv:2103.11814 [hep-ph]

    2021 arXiv

  244. [252]

    De Romeri, K

    V. De Romeri, K. J. Kelly, and P. A. N. Machado, Phys. Rev. D100, 095010 (2019), arXiv:1903.10505 [hep-ph]

    2019 arXiv

  245. [253]

    Breitbach, L

    M. Breitbach, L. Buonocore, C. Frugiuele, J. Kopp, and L. Mittnacht, JHEP01, 048 (2022), arXiv:2102.03383 [hep-ph]

    2022 arXiv

  246. [254]

    Alonsoet al., Phys

    J. Alonsoet al., Phys. Rev. D105, 052009 (2022), arXiv:2111.09480 [hep-ex]

    2022 arXiv

  247. [255]

    Atifet al.(RENO, NEOS), Phys

    Z. Atifet al.(RENO, NEOS), Phys. Rev. D105, L111101 (2022), arXiv:2011.00896 [hep-ex]

    2022

  248. [256]

    Rene tdr [manuscript submitted for publication],

    RENE (RENE), “Rene tdr [manuscript submitted for publication],”

  249. [257]

    Anet al.(JUNO), J

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

    2016 arXiv

  250. [258]

    Abuslemeet al.(JUNO), Prog

    A. Abuslemeet al.(JUNO), Prog. Part. Nucl. Phys.123, 103927 (2022), arXiv:2104.02565 [hep-ex]

    2022

  251. [259]

    Abuslemeet al.(JUNO), Chin

    A. Abuslemeet al.(JUNO), Chin. Phys. C49, 033104 (2025), arXiv:2405.18008 [hep-ex]

    2025

  252. [260]

    Abuslemeet al.(JUNO), Chin

    A. Abuslemeet al.(JUNO), Chin. Phys. C46, 123001 (2022), arXiv:2204.13249 [hep-ex]

    2022

  253. [261]

    Abuslemeet al.(JUNO), (2020), arXiv:2005.08745 [physics.ins-det]

    A. Abuslemeet al.(JUNO), (2020), arXiv:2005.08745 [physics.ins-det]

    2020

  254. [262]

    Nakamura, H

    R. Nakamura, H. Sambonsugi, K. Shiraishi, and Y. Wada, J. Phys. Conf. Ser.1468, 012256 (2020)

    2020

  255. [263]

    Kim (AMoRE), PoSICHEP2024, 133 (2025)

    W. Kim (AMoRE), PoSICHEP2024, 133 (2025)

    2025

  256. [264]

    D. R. Nygren,1974 PEP summer study, PEP Summar Study ProceedingsC740805, 58 (1974)

    1974

  257. [265]

    Amerioet al., Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment527, 329 (2004)

    S. Amerioet al., Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment527, 329 (2004)

    2004

  258. [266]

    Bakhti and A

    P. Bakhti and A. Y. Smirnov, Phys. Rev. D101, 123031 (2020), arXiv:2001.08030 [hep-ph]

    2020 arXiv

  259. [267]

    Kim, J.-C

    D. Kim, J.-C. Park, and S. Shin, Phys. Rev. D100, 035033 (2019), arXiv:1903.05087 [hep-ph]

    2019 arXiv

  260. [268]

    Berger, Y

    J. Berger, Y. Cui, M. Graham, L. Necib, G. Petrillo, D. Stocks, Y.-T. Tsai, and Y. Zhao, Phys. Rev. D103, 095012 (2021), arXiv:1912.05558 [hep-ph]

    2021 arXiv

  261. [269]

    Abeet al.(Hyper-Kamiokande), (2018), arXiv:1805.04163 [physics.ins-det]

    K. Abeet al.(Hyper-Kamiokande), (2018), arXiv:1805.04163 [physics.ins-det]

    2018 arXiv

  262. [270]

    M. Du, R. Fang, Z. Liu, W. Lu, and Z. Ye, (2023), arXiv:2308.05607 [hep-ph]

    2023 arXiv

  263. [271]

    N. F. Bell, M. J. Dolan, and S. Robles, JCAP11, 004 (2021), arXiv:2107.04216 [hep-ph]

    2021 arXiv

  264. [272]

    Primulando and P

    R. Primulando and P. Uttayarat, JHEP06, 026 (2018), arXiv:1710.08567 [hep-ph]

    2018 arXiv

  265. [273]

    Olivares-Del Campo, C

    A. Olivares-Del Campo, C. Bœhm, S. Palomares-Ruiz, and S. Pascoli, Phys. Rev. D97, 075039 (2018), arXiv:1711.05283 [hep-ph]

    2018 arXiv

  266. [274]

    Olivares-Del Campo, S

    A. Olivares-Del Campo, S. Palomares-Ruiz, and S. Pascoli, in53rd Rencontres de Moriond on Elec- troweak Interactions and Unified Theories(2018) pp. 441–444, arXiv:1805.09830 [hep-ph]

    2018 arXiv

  267. [275]

    Blennow, E

    M. Blennow, E. Fernandez-Martinez, A. Olivares-Del Campo, S. Pascoli, S. Rosauro-Alcaraz, and A. V. Titov, Eur. Phys. J. C79, 555 (2019), arXiv:1903.00006 [hep-ph]

    2019 arXiv

  268. [276]

    Palomares-Ruiz and S

    S. Palomares-Ruiz and S. Pascoli, Phys. Rev. D77, 025025 (2008), arXiv:0710.5420 [astro-ph]

    2008 arXiv

  269. [277]

    N. F. Bell, M. J. Dolan, and S. Robles, JCAP09, 019 (2020), arXiv:2005.01950 [hep-ph]

    2020 arXiv

  270. [278]

    Ishihara (IceCube), PoSICRC2019, 1031 (2021), arXiv:1908.09441 [astro-ph.HE]

    A. Ishihara (IceCube), PoSICRC2019, 1031 (2021), arXiv:1908.09441 [astro-ph.HE]

    2021 arXiv

  271. [279]

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

    2021

  272. [280]

    M. G. Aartsenet al.(IceCube), Nature551, 596 (2017), arXiv:1711.08119 [hep-ex]

    2017 arXiv

  273. [281]

    V. B. Valera, M. Bustamante, and C. Glaser, PoSICRC2023, 1063 (2023), arXiv:2307.11050 [hep- ph]

    2023 arXiv

  274. [282]

    Ladet al.(IceCube-Gen2), PoSICRC2023, 1123 (2023), arXiv:2308.15220 [astro-ph.HE]

    N. Ladet al.(IceCube-Gen2), PoSICRC2023, 1123 (2023), arXiv:2308.15220 [astro-ph.HE]

    2023 arXiv

  275. [283]

    Abuslemeet al.(JUNO), JCAP10, 033 (2022), arXiv:2205.08830 [hep-ex]

    A. Abuslemeet al.(JUNO), JCAP10, 033 (2022), arXiv:2205.08830 [hep-ex]

    2022

  276. [284]

    Abuslemeet al.(JUNO), JCAP01, 057 (2024), arXiv:2309.07109 [hep-ex]

    A. Abuslemeet al.(JUNO), JCAP01, 057 (2024), arXiv:2309.07109 [hep-ex]

    2024

  277. [285]

    Abuslemeet al.(JUNO), JHEP11, 102 (2021), arXiv:2107.03669 [physics.ins-det]

    A. Abuslemeet al.(JUNO), JHEP11, 102 (2021), arXiv:2107.03669 [physics.ins-det]

    2021

  278. [286]

    Abuslemeet al.(JUNO), Chin

    A. Abuslemeet al.(JUNO), Chin. Phys. C45, 023004 (2021), arXiv:2006.11760 [hep-ex]. 51

    2021

  279. [287]

    Zhaoet al.(JUNO), Astrophys

    J. Zhaoet al.(JUNO), Astrophys. J.965, 122 (2024), arXiv:2210.08437 [hep-ex]

    2024

  280. [288]

    Abuslemeet al.(JUNO), JCAP10, 022 (2023), arXiv:2303.03910 [hep-ex]

    A. Abuslemeet al.(JUNO), JCAP10, 022 (2023), arXiv:2303.03910 [hep-ex]

    2023

  281. [289]

    Guo, JCAP01, 039 (2016), arXiv:1511.04888 [hep-ph]

    W.-L. Guo, JCAP01, 039 (2016), arXiv:1511.04888 [hep-ph]

    2016 arXiv

  282. [290]

    Smirnov, G

    M. Smirnov, G. Yang, J. Liao, Z. Hu, and J. Ling, Phys. Rev. D104, 116024 (2021), arXiv:2109.04276 [hep-ex]

    2021 arXiv

  283. [291]

    van Remortel, M

    N. van Remortel, M. Colomer Molla, B. Clerbaux, A. De Roeck, M. Drewes, R. Keloth, H. Sfar, S. Vercaemer, and M. Verstraeten, JHEP07, 128 (2024), arXiv:2403.04662 [hep-ph]

    2024 arXiv

  284. [292]

    Lucente, N

    G. Lucente, N. Nath, F. Capozzi, M. Giannotti, and A. Mirizzi, Phys. Rev. D106, 123007 (2022), arXiv:2209.11780 [hep-ph]

    2022 arXiv

  285. [293]

    Abuslemeet al.(JUNO), Chin

    A. Abuslemeet al.(JUNO), Chin. Phys. C47, 113002 (2023), arXiv:2212.08502 [hep-ex]

    2023

  286. [294]

    Abuslemeet al.(JUNO), Eur

    A. Abuslemeet al.(JUNO), Eur. Phys. J. C85, 5 (2025), arXiv:2405.17792 [hep-ex]

    2025

  287. [295]

    Zhao, L.-J

    J. Zhao, L.-J. Wen, Y.-F. Wang, and J. Cao, Chin. Phys. C41, 053001 (2017), arXiv:1610.07143 [hep-ex]

    2017 arXiv

  288. [296]

    Cao, G.-Y

    J. Cao, G.-Y. Huang, Y.-F. Li, Y. Wang, L.-J. Wen, Z.-Z. Xing, Z.-H. Zhao, and S. Zhou, Chin. Phys. C44, 031001 (2020), arXiv:1908.08355 [hep-ph]

    2020 arXiv

  289. [297]

    Ding, M.-C

    Y.-Y. Ding, M.-C. Liu, L.-J. Wen, Y.-x. Li, G.-s. Li, and Z.-y. Zhang, Nucl. Instrum. Meth. A1049, 168111 (2023)

    2023

  290. [298]

    Agostiniet al.(BOREXINO), Nature562, 505 (2018)

    M. Agostiniet al.(BOREXINO), Nature562, 505 (2018)

    2018

  291. [299]

    Appelet al.(BOREXINO), Phys

    S. Appelet al.(BOREXINO), Phys. Rev. Lett.129, 252701 (2022), arXiv:2205.15975 [hep-ex]

    2022 arXiv

  292. [300]

    Al Kharusiet al.(SNEWS), New J

    S. Al Kharusiet al.(SNEWS), New J. Phys.23, 031201 (2021), arXiv:2011.00035 [astro-ph.HE]

    2021 arXiv

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.