Anomalies in neutrino oscillations and Physics BSM

University of Bari & INFN Anomalies in n oscillations and Physics BSM Antonio Palazzo NeuTel 2025 1.10.2025 Introduction Outline 01/10/2025 2Antonio Palazzo, UNIBA & INFN Neutrino anomalies across baselines and their interpretation in the 3+1 scheme Possible role of new matter effects in NOvA and T2K Conclusions δ m2/eV2~ 7.34 x 10-5 ±2.2% Δ m2/eV2 ~ 2.48 x 10-3 ±1.3% sin2 θ 12 ~ 0.303 ±4.4% sin2 θ 13 ~0.0225 ±3.8% sin2 θ 23 ~0.545 ±5.0% 01/10/2025 10! solar model prediction. Continued data-taking refined these results. Data-taking was concluded in 2006 and the final results were published in 2013 [35]. The 8B neutrino flux from the final fit to all reactions is !!!! € φ = φ ( ν e)+ φ ( ν µ )+ φ ( ν τ )=5.25±0.16(stat)−0.13 +0.11 (sys)×106cm−2s−1 in very good agreement with the theoretically expected 5.94 (1 ± 0.11) [SSM BPS08] or 5.58 (1 ± 0.14) [SSM SHP11] (see [36] and references therein). The flux of muonand tau-neutrinos deduced from the results shown in figure 4 is !! € φ ( ν µ )+ φ ( ν τ )=(3.26±0.25 −0.35 +0.40 )×10 6 cm −2 s −1 deviating significantly from zero. A comparison with the total 8B flux clearly demonstrates that about two thirds of the solar electron-neutrinos changed flavour, arriving at Earth as muon-neutrinos or tau-neutrinos. SNO’s ES results are consistent with the results from SuperKamiokande and with the SNO results above, however by themselves insufficient as evidence for flavour change (figure 4). Figure 4: Fluxes of 8B solar neutrinos from SNO and Super-Kamiokande. The SSM BS05 [38] prediction is shown as a range between the dashed lines. C.L. stands for confidence level. From [36] and references therein. The SNO evidence for neutrino flavour conversion was confirmed a year later by the KamLAND reactor experiment. KamLAND (Kamioka Liquid scintillator AntiNeutrino Detector) [39] was proposed in 1994, funded in 1997 and started data-taking in January 2002. The first KamLAND results were published in January 2003 [40] and show clear evidence for disappearance of electron anti-neutrinos, consistent with the expectation from the solar Discoveries Super-K 95% Cl 95% Ga 95% νµ↔ντ νe↔νX 100 10–3 ∆m2 [eV2] 10–12 10–9 10–6 102 100 10–2 10–4 tan2θ CHOOZ Bugey CHORUS NOMAD CHORUS KARMEN2 νe↔ντ NOMAD νe↔νµ CDHSW NOMAD KamLAND 95% SNO 95% Super-K 95% all solar 95% http://hitoshi.berkeley.edu/neutrino SuperK All limits are at 90%CL unless otherwise noted LSND 90/99% MiniBooNE K2K MINOS T2K OPERA ICARUS Daya Bay 95% Interpretation known knowns Oustanding progress in n physics in ~ 25 years + many other ones: solar, KamLAND, q13 at reactors & T2K … d(CP) sign( D m2) octant( q 23) absolute nmass Dirac/Majorana NSI, sterile states, PMNS non-unitarity, ...? known unknowns unkown unknowns 3 3-flavor scheme now established as the standard framework… 3Antonio Palazzo, UNIBA & INFN NO IO ? n 3 The 3nmass spectrum or n 2 n 1 nenµnt dm2 +Dm2 -Dm2 sub-eV n 3 Likely NO (?) Dm2 dm2 =0.03 a = 01/10/2025 4Antonio Palazzo, UNIBA & INFN Dirac CP-violating phase d The 3nmixing matrix Explicit form q23 ~ 45º q13 ~ 9ºq12 ~ 34º U is non-real if d≠ (0, p) Three non-zero qij: Way open to CPV searches… 01/10/2025 5Antonio Palazzo, UNIBA & INFN 01/10/2025 6 6 6.5 7.0 7.5 8.0 8.5 0 1 2 3 4 2.2 2.3 2.4 2.5 2.6 2.7 0 1 2 3 4 0.0 0.5 1.0 1.5 2.0 0 1 2 3 4 0.25 0.30 0.35 0 1 2 3 4 0.01 0.02 0.03 0.04 0 1 2 3 4 0.3 0.4 0.5 0.6 0.7 0 1 2 3 4 6.5 7.0 7.5 8.0 8.5 ] 2 eV -5 [10 2 mδ ] 2 eV -5 [10 2 mδ 0 1 2 3 4 σN σN 2.2 2.3 2.4 2.5 2.6 2.7 ] 2 eV -3 [10 2 mΔ ] 2 eV -3 [10 2 mΔ σN σN 0.0 0.5 1.0 1.5 2.0 π/δ π/δ σN σN 0.25 0.30 0.35 12 θ 2 sin 12 θ 2 sin 0 1 2 3 4 σN σN 0.01 0.02 0.03 0.04 13 θ 2 sin 13 θ 2 sin σN σN 0.3 0.4 0.5 0.6 0.7 23 θ 2 sin 23 θ 2 sin σN σN LBL Acc + Solar + KamLAND + SBL Reactors + Atmos σN σN NO IO FIG. 3: As in Fig. 2, but adding atmospheric ⌫data (i.e., with all oscillation data included). NO is favored at 2.2. Summarizing, in the last few years there has been an appreciable progress on three known oscillation parameters (|m2|,✓ 13,✓ 23), with the first one entering the subpercent precision era. Previous hints about the three oscillation unknowns (✓23 octant, CP phase , mass ordering) are instead weaker. Finally, we note that our global results (Fig. 3 and Table I) are in good agreement with ones reported in an independent analysis [15]. The agreement would be even better by excluding the recent RENO data [33] appeared after [15]; in particular, we would then obtain a preference for NO at 2.5as in [15]. TABLE I: Global 3⌫oscillation analysis: best-fit values and allowed ranges at N= 1, 2, 3, for either NO or IO. The last column shows the formal “1parameter accuracy,” defined as 1/6 of the 3range, divided by the best-fit value (in percent). We recall that m2=m2 3(m2 1+m2 2)/2 and that /⇡is cyclic (mod 2). Last row: 2o↵set between IO and NO. Parameter Ordering Best fit 1range 2range 3range “1”(%) m2/105eV2NO, IO 7.37 7.21 – 7.52 7.06 – 7.71 6.93 – 7.93 2.3 sin2✓12/101NO, IO 3.03 2.91 – 3.17 2.77 – 3.31 2.64 – 3.45 4.5 |m2|/103eV2NO 2.495 2.475 – 2.515 2.454 – 2.536 2.433 – 2.558 0.8 IO 2.465 2.444 – 2.485 2.423 – 2.506 2.403 – 2.527 0.8 sin2✓13/102NO 2.23 2.17 – 2.27 2.11 – 2.33 2.06 – 2.38 2.4 IO 2.23 2.19 – 2.30 2.14 – 2.35 2.08 – 2.41 2.4 sin2✓23/101NO 4.73 4.60 – 4.96 4.47 – 5.68 4.37 – 5.81 5.1 IO 5.45 5.28 – 5.60 4.58 – 5.73 4.43 – 5.83 4.3 /⇡NO 1.20 1.07 – 1.37 0.88 – 1.81 0.73 – 2.03 18 IO 1.48 1.36 – 1.61 1.24 – 1.72 1.12 – 1.83 8 2 IONO IONO +5.0 Antonio Palazzo, UNIBA & INFN Entering the precision era Capozzi et al. arXiv:2503.07752 [hep-ph] PRD 111, 0993006 (2025) The right moment to look for cracks in the model 01/10/2025 The 3+1 scheme 7Antonio Palazzo, UNIBA & INFN |Us4| ~1 Dmsol Dmatm 2 2 3n scheme 3+1 scheme Minimal extension of 3-flavor scheme Dm14 ~ 1 eV2 2 01/10/2025 Sterile neutrinos are truly sterile (only mixing) 88Antonio Palazzo, UNIBA & INFN Sterile ns bring new CPV sources U = R34 R24 R14 R23 R13 R12 ∼ charged current part, the Lagrangian is invariant under the following global phase transformations: ⇧kL ⇤ei⇧k⇧kL,⇧kR ⇤ei⇧k⇧kR (k=1,2,3) (66) L⇤ei⇧L,R⇤ei⇧R(=e, µ, ⌃) (67) A3⇥3 Dirac mixing matrix therefore depends on three mixing angles and one CPviolating phase. In the Majorana case, the mass term is not invariant under the phase transformation in equation 66. Hence in the Majorana case, the mixing matrix depends on two extra Majorana phases, which makes three mixing angles and three CP-violating phases. In this case, the mixing matrix can be written as U=UDDM(68) where UDis the mixing matrix of the Dirac case and DMis a diagonal unitary matrix with two independent phases: DM= diag(ei⌅1,e i⌅2,e i⌅3),⇤1=0.(69) The oscillation probability however is independent of the Majorana phases. The mixing matrix elements in the Majorana case are written as Uk=UD kei⌅k.(70) The product of the mixing matrix that appears in the oscillation probability therefore becomes U⇥ kU⇥kUjU⇥ ⇥j=UD⇥ kei⌅kUD ⇥kei⌅kUD jei⌅jUD⇥ ⇥jei⌅j=UD⇥ kUD ⇥kUD jUD⇥ ⇥j.(71) Hence, neutrino oscillations do not depend on the Majorana phases and the Majorana phases cannot be measured by neutrino oscillation experiments. The oscillation probability for Dirac and Majorana neutrinos is identical, so from now on we will not treat them as different cases anymore. The mixing matrix Ucan be parameterized by the multiplication of the real orthogonal matrices Rjk. These matrices perform a rotation of an angle ⇥jk in the j–k plane. For a2⇥2 matrix, they are simply given by: Rij =cij sij sij cij ⇥,˜ Rij =cij ˜sij ˜s⇥ ij cij ⇥(72) sij =sin⇥ij ˜sij =sijei⇤ij cij =cos⇥ij For mixing matrices with higher dimensions, the matrices Rjk can be constructed from: 19 charged current part, the Lagrangian is invariant under the following global phase transformations: ⇧kL ⇤ei⇧k⇧kL,⇧kR ⇤ei⇧k⇧kR (k=1,2,3) (66) L⇤ei⇧L,R⇤ei⇧R(=e, µ, ⌃) (67) A3⇥3 Dirac mixing matrix therefore depends on three mixing angles and one CPviolating phase. In the Majorana case, the mass term is not invariant under the phase transformation in equation 66. Hence in the Majorana case, the mixing matrix depends on two extra Majorana phases, which makes three mixing angles and three CP-violating phases. In this case, the mixing matrix can be written as U=UDDM(68) where UDis the mixing matrix of the Dirac case and DMis a diagonal unitary matrix with two independent phases: DM= diag(ei⌅1,e i⌅2,e i⌅3),⇤1=0.(69) The oscillation probability however is independent of the Majorana phases. The mixing matrix elements in the Majorana case are written as Uk=UD kei⌅k.(70) The product of the mixing matrix that appears in the oscillation probability therefore becomes U⇥ kU⇥kUjU⇥ ⇥j=UD⇥ kei⌅kUD ⇥kei⌅kUD jei⌅jUD⇥ ⇥jei⌅j=UD⇥ kUD ⇥kUD jUD⇥ ⇥j.(71) Hence, neutrino oscillations do not depend on the Majorana phases and the Majorana phases cannot be measured by neutrino oscillation experiments. The oscillation probability for Dirac and Majorana neutrinos is identical, so from now on we will not treat them as different cases anymore. The mixing matrix Ucan be parameterized by the multiplication of the real orthogonal matrices Rjk. These matrices perform a rotation of an angle ⇥jk in the j–k plane. For a2⇥2 matrix, they are simply given by: Rij =cij sij sij cij ⇥,˜ Rij =cij ˜sij ˜s⇥ ij cij ⇥(72) sij =sin⇥ij ˜sij =sijei⇤ij cij =cos⇥ij For mixing matrices with higher dimensions, the matrices Rjk can be constructed from: 19 charged current part, the Lagrangian is invariant under the following global phase transformations: ⇧kL ⇤ei⇧k⇧kL,⇧kR ⇤ei⇧k⇧kR (k=1,2,3) (66) L⇤ei⇧L,R⇤ei⇧R(=e, µ, ⌃) (67) A3⇥3 Dirac mixing matrix therefore depends on three mixing angles and one CPviolating phase. In the Majorana case, the mass term is not invariant under the phase transformation in equation 66. Hence in the Majorana case, the mixing matrix depends on two extra Majorana phases, which makes three mixing angles and three CP-violating phases. In this case, the mixing matrix can be written as U=UDDM(68) where UDis the mixing matrix of the Dirac case and DMis a diagonal unitary matrix with two independent phases: DM= diag(ei⌅1,e i⌅2,e i⌅3),⇤1=0.(69) The oscillation probability however is independent of the Majorana phases. The mixing matrix elements in the Majorana case are written as Uk=UD kei⌅k.(70) The product of the mixing matrix that appears in the oscillation probability therefore becomes U⇥ kU⇥kUjU⇥ ⇥j=UD⇥ kei⌅kUD ⇥kei⌅kUD jei⌅jUD⇥ ⇥jei⌅j=UD⇥ kUD ⇥kUD jUD⇥ ⇥j.(71) Hence, neutrino oscillations do not depend on the Majorana phases and the Majorana phases cannot be measured by neutrino oscillation experiments. The oscillation probability for Dirac and Majorana neutrinos is identical, so from now on we will not treat them as different cases anymore. The mixing matrix Ucan be parameterized by the multiplication of the real orthogonal matrices Rjk. These matrices perform a rotation of an angle ⇥jk in the j–k plane. For a2⇥2 matrix, they are simply given by: Rij =cij sij sij cij ⇥,˜ Rij =cij ˜sij ˜s⇥ ij cij ⇥(72) sij =sin⇥ij ˜sij =sijei⇤ij cij =cos⇥ij For mixing matrices with higher dimensions, the matrices Rjk can be constructed from: 19 charged current part, the Lagrangian is invariant under the following global phase transformations: ⇧kL ⇤ei⇧k⇧kL,⇧kR ⇤ei⇧k⇧kR (k=1,2,3) (66) L⇤ei⇧L,R⇤ei⇧R(=e, µ, ⌃) (67) A3⇥3 Dirac mixing matrix therefore depends on three mixing angles and one CPviolating phase. In the Majorana case, the mass term is not invariant under the phase transformation in equation 66. Hence in the Majorana case, the mixing matrix depends on two extra Majorana phases, which makes three mixing angles and three CP-violating phases. In this case, the mixing matrix can be written as U=UDDM(68) where UDis the mixing matrix of the Dirac case and DMis a diagonal unitary matrix with two independent phases: DM= diag(ei⌅1,e i⌅2,e i⌅3),⇤1=0.(69) The oscillation probability however is independent of the Majorana phases. The mixing matrix elements in the Majorana case are written as Uk=UD kei⌅k.(70) The product of the mixing matrix that appears in the oscillation probability therefore becomes U⇥ kU⇥kUjU⇥ ⇥j=UD⇥ kei⌅kUD ⇥kei⌅kUD jei⌅jUD⇥ ⇥jei⌅j=UD⇥ kUD ⇥kUD jUD⇥ ⇥j.(71) Hence, neutrino oscillations do not depend on the Majorana phases and the Majorana phases cannot be measured by neutrino oscillation experiments. The oscillation probability for Dirac and Majorana neutrinos is identical, so from now on we will not treat them as different cases anymore. The mixing matrix Ucan be parameterized by the multiplication of the real orthogonal matrices Rjk. These matrices perform a rotation of an angle ⇥jk in the j–k plane. For a2⇥2 matrix, they are simply given by: Rij =cij sij sij cij ⇥,˜ Rij =cij ˜sij ˜s⇥ ij cij ⇥(72) sij =sin⇥ij ˜sij =sijei⇤ij cij =cos⇥ij For mixing matrices with higher dimensions, the matrices Rjk can be constructed from: 19 charged current part, the Lagrangian is invariant under the following global phase transformations: ⇧kL ⇤ei⇧k⇧kL,⇧kR ⇤ei⇧k⇧kR (k=1,2,3) (66) L⇤ei⇧L,R⇤ei⇧R(=e, µ, ⌃) (67) A3⇥3 Dirac mixing matrix therefore depends on three mixing angles and one CPviolating phase. In the Majorana case, the mass term is not invariant under the phase transformation in equation 66. Hence in the Majorana case, the mixing matrix depends on two extra Majorana phases, which makes three mixing angles and three CP-violating phases. In this case, the mixing matrix can be written as U=UDDM(68) where UDis the mixing matrix of the Dirac case and DMis a diagonal unitary matrix with two independent phases: DM= diag(ei⌅1,e i⌅2,e i⌅3),⇤1=0.(69) The oscillation probability however is independent of the Majorana phases. The mixing matrix elements in the Majorana case are written as Uk=UD kei⌅k.(70) The product of the mixing matrix that appears in the oscillation probability therefore becomes U⇥ kU⇥kUjU⇥ ⇥j=UD⇥ kei⌅kUD ⇥kei⌅kUD jei⌅jUD⇥ ⇥jei⌅j=UD⇥ kUD ⇥kUD jUD⇥ ⇥j.(71) Hence, neutrino oscillations do not depend on the Majorana phases and the Majorana phases cannot be measured by neutrino oscillation experiments. The oscillation probability for Dirac and Majorana neutrinos is identical, so from now on we will not treat them as different cases anymore. The mixing matrix Ucan be parameterized by the multiplication of the real orthogonal matrices Rjk. These matrices perform a rotation of an angle ⇥jk in the j–k plane. For a2⇥2 matrix, they are simply given by: Rij =cij sij sij cij ⇥,˜ Rij =cij ˜sij ˜s⇥ ij cij ⇥(72) sij =sin⇥ij ˜sij =sijei⇤ij cij =cos⇥ij For mixing matrices with higher dimensions, the matrices Rjk can be constructed from: 19 ∼ ∼ { 3n 3 mixing angles 1 Dirac phases 2 Majorana phases 3+3N 1+2N 2+N 3+N3n { { 6 3 3 3+1 { 01/10/2025 Invisible at SBL but visible at LBL experiments 9Antonio Palazzo, UNIBA & INFN 01/10/2025 16 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 (GeV) QE ν E 0 1 2 3 4 5 Events/MeV Data (stat err.) +/- µ from e ν+/- from K e ν0 from K e ν misid 0 π γ N→ Δ dirt other Constr. Syst. Error Best Fit 3.0 (MeV) ν Reconstructed E 0 500 1000 1500 2000 2500 Events/100 MeV 0 5 10 15 20 25 30 35 40 45 POT 20 10×MicroBooNE 6.369 BNB data, 338 Pred. uncertainty Others, 10.0 NC, 22.5 CC, 19.3 µ ν CC, 333.1 e ν eLEE Model (x=1), 37.0 a) b) Figure 3.4: (Left) Observed low-energy excess of ⌫e-like events in the MiniBooNE experiment [95]. The significance of the excess is about 4.8 . (Right) The search for a low-energy excess in the inclusive ⌫echarged-current interactions in the MicroBooNE experiment [97] using the same Booster Neutrino Beam at Fermilab as in MiniBooNE. The numbers in the legend show the total number of selected candidates and predicted events in each category. Since no low-energy excess was observed in MicroBooNE, the hypothesis that the low-energy excess observed in MiniBooNE are all from ⌫es is disfavored at over 2.6 . 4experimentin2020claimedanobservationofreactor¯⌫eoscillations in the range of 6–12 meters with the expected L/E dependence driven by a eV-mass-scale sterile neutrino [114], but it has not yet been independently confirmed by other reactor antineutrino experiments searching for similar spectral shape distortion at varying baselines. Figure 3.6 summarizes the current status in searching for a sterile neutrino induced (anti-)⌫edisappearance oscillation. For m2 41 below 10 eV2, a large portion of the allowed regions from the Gallium anomaly (GALLEX+SAGE+BEST) and the Neutrino-4 anomaly has been excluded by direct searches from short-baseline reactor antineutrino experiments: PROSPECT [40], STEREO [115], DANSS [116], the combined analysis of RENO and NEOS [117], and the MicroBooNE [103]experiment. The high m2 41 region has been significantly constrained by KATRIN’s limit on the neutrino mass through the measurement of electron energy spectrum near tritium -decay end-point [118]. At the same time, the allowed regions are also in strong tension with the solar neutrino measurements [119]andthefirstrowofPMNSmatrixbeingconsistent with unitary [120,121]. While the observed experimental anomalies have not yet been completely resolved, the simple explanation with sterile neutrino oscillations (i.e. the 3 active +1sterileneutrinomodel)isnolongerappealing. An alternative solution to the RAA resorts to nuclear physics. Additional uncertainties could affect the original cumulative beta spectra that the conversion method is based on. For instance, some (n, e)reactioncrosssectionsand internal conversion coefficients used in the ILL measurements for the calibration and normalization of the beta spectra to the total number of fissions have been revised since the experiments [122]. The recent measurement of the -spectrum ratio between 235Uand239Pu at the Kurchatov Institute (KI) [123]alsosuggeststhattherecouldbeanissueinthe original ILL measurements (see details in Sec. 4.3). Another avenue is the procedure for adjusting the conversion method itself, whose systematic uncertainties are questionable. Depending on the adopted average effective Z distributions used in the fit of the ILL spectra, converted spectra could vary by 1% [124]. Moreover, known nuclear structure elements, in particular the contributions of non-unique forbidden transitions, could significantly increase the published systematic uncertainty and distort the converted ¯⌫espectrum. Indeed, forbidden transitions contribute to 30% of the total spectrum, and they dominate the spectrum beyond 4 MeV. Several theoretical works have tried to estimate the potential uncertainties 25 2 due to the awesome reconstruction power of Liquid Argon Time Projection Chambers (LArTPCs). In addition, MiniBooNE has reported an excess of electron neutrino candidate events [8] that seem to require an explanation beyond a m4⇠1 eV sterile neutrino due to constraints from MicroBooNE, MINOS+, IceCube, and cosmology [12,13,28,41–44], some of which could potentially be evaded in more complicated models [31–40,49,50]. It is still to be determined if existing explanations of MiniBooNE without a m4⇠1 eV sterile neutrino [51–61] are also consistent with MicroBooNE’s new results; until this story is better understood it does not make statistical sense to analyze the MiniBooNE data for ⌫edisappearance. In this letter we will present a ⌫edisappearance sterile oscillation analysis of the MicroBooNE data focusing on the Wire-Cell analysis in section II, compare the result to others in the literature, and discuss the results. The analysis of the other three channels can be found in appendix B. Next, we will compare the MicroBooNE results to others in the literature in section III. We then discuss our results and conclude in section IV and V. All the data files associated the parameter scans shown in fig. 2and appendix Bcan be found at peterdenton.github.io/Data/Micro Dis/index.html. II. ANALYSIS MicroBooNE has reported four ⌫eanalyses dubbed: Wire-Cell [44] which is sensitive to final states with one electron and anything else including both fully and partially contained events, Pandora [43] which is sensitive to final states with one electron, zero pions, and either zero protons or 1+ protons, and Deep-Learning [42]which is sensitive to final states with one electron and one proton, primarily from charged-current quasi-elastic interactions. Each of these four analyses has di↵erent strengths and weaknesses in terms of statistics, purity, and calibration data summarized in [41]. As the Wire-Cell analysis has the highest ⌫estatistics, we take it as our fiducial analysis, but we also investigate the other channels for completeness, see appendix B. To analyze the MicroBooNE data in terms of a sterile neutrino, we consider a two parameter model where the sterile neutrino mixes dominantly with electron neutrinos. Thus the expected ⌫eevents will be reduced by the disappearance probability, P(⌫e!⌫e)=1sin2(2✓14)sin 2✓m2 41L 4E◆,(1) where L= 470 m is MicroBooNE baseline [46], m2 41 ⌘ m2 4m2 1is the new oscillation frequency, and ✓14 gives the amplitude of the oscillations. This is equivalent to setting ✓24 =✓34 = 0, or to small enough values to be irrelevant. While a full analysis including a combination of all channels, a full treatment of energy reconstruction, backFIG. 1. Top: The disappearance probability in true energy for the best fit set of sterile oscillation parameters, m2 41 =1.25 eV2and sin2(2✓14)=0.35, for the Wire-Cell data. Bottom: The expected event rate at MicroBooNE in the Wire-Cell analysis in reconstructed neutrino energy [44] including contributions from backgrounds (red) and ⌫eevents (green) along with the systematic uncertainty (gray hatched). The actual data is shown in black and the expected data, assuming the best fit sterile hypothesis, is shown in orange. 102101100 sin2(214) 101 100 101 102 103 m2 41 [eV2] Wire-Cell Best fit: sin2(2✓14)=0.35 m2 41 =1.25 eV2 FC : p=0.015 2.4 Wilks Best fit 1 2 FIG. 2. The preferred regions in m2 41 -sin 2(2✓14) parameter space using data from MicroBooNE’s Wire-Cell analysis [44]. The blue (orange) contours are at 1(2) as determined by Wilks’ theorem; the Feldman-Cousins significance of the best fit compared to no oscillations is 2.4with a simplified treatment of systematics. grounds, and other systematics is necessary to robustly quantify the statistical significance of these sterile oscillations, we can still get a good estimate of the parameters of interest preferred in a simplified analysis. In order to Hint of nedisappearance in MicroBooNE P. B. Denton arXiv: 2111.05793 [hep-ph] PRL 129, 061801 (2022) MicroBooNE arXiv: 2110.14054 [hep-ex] PRL 128, 241801 (2022) Note: ONLY disappearance (no app. considered) Antonio Palazzo, UNIBA & INFN 01/10/2025 17 Hint vanishes in the 3+1 scheme MicroBooNE arXiv: 2210.10216 [hep-ex] PRL 130, 011801 (2023) 6 4− 10 3− 10 2− 10 1− 10 1 eµ θ2 2 sin 2− 10 1− 10 1 10 2 10 ) 2 (eV 41 2 mΔ LSND 90% CL (allowed) LSND 99% CL (allowed) POT 20 10×MicroBooNE 6.369 s 95% CL Data, profiling Sensitivity, profiling App. only e νSensitivity, (a) 2− 10 1− 10 1 ee θ2 2 sin 1− 10 1 10 ) 2 (eV 41 2 mΔ GALLEX+SAGE+BEST (allowed)σ2 (allowed)σNeutrino-4 2 s 95% CL Data, profiling Sensitivity, profiling Disapp. only e νSensitivity, POT 20 10×MicroBooNE 6.369 (b) FIG. 2. MicroBooNE CLsexclusion contours at the 95% CL in the plane of m2 41 and (a) sin22✓µeor (b) sin22✓ee. The red solid (dashed) curve represents the MicroBooNE 95% CLsdata exclusion (Asimov sensitivity) limits after profiling over the mixing angle sin2✓24. The blue long-dashed curve represents the MicroBooNE 95% CLsAsimov sensitivity in the scenario of (a) ⌫eappearance-only or (b) ⌫edisappearance-only as opposed to the full 3 + 1 oscillation result. In (a), the LSND 90% and 99% CL allowed regions [25] using the ⌫eappearance-only approximation are shown as the light blue and gray shaded areas, respectively. In (b), the cyan shaded area represents the 2allowed region of the gallium anomaly from the experimental results of GALLEX, SAGE, and BEST [20]. The 2allowed region of the Neutrino-4 experiment [24] is also shown in (b). show no evidence of sterile neutrino oscillations and are found to be consistent with the 3⌫hypothesis within 1significance. The current exclusion contours, corresponding to a BNB exposure of 6.369⇥1020 POT, allow for a test of part of the sterile neutrino parameter space suggested by other experimental anomalies. This result provides the first constraints, competitive in the relatively high m2 41 region, on the eV-scale sterile neutrino parameter space measured in a LArTPC detector from an accelerator neutrino source. This work paves the way for future neutrino oscillation searches with LArTPCs in the SBN and DUNE [81] experiments. An upcoming search for sterile neutrino oscillations at MicroBooNE combining the BNB and NuMI data will improve upon the current result by breaking the parameter degeneracy in some regions and by using data from two di↵erent beamlines. This document was prepared by the MicroBooNE collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, Office of Science, HEP User Facility. Fermilab is managed by Fermi Research Alliance, LLC (FRA), acting under Contract No. DE-AC02-07CH11359. MicroBooNE is supported by the following: the U.S. Department of Energy, Office of Science, Offices of High Energy Physics and Nuclear Physics; the U.S. National Science Foundation; the Swiss National Science Foundation; the Science and Technology Facilities Council (STFC), part of the United Kingdom Research and Innovation; the Royal Society (United Kingdom); and the UK Research and Innovation (UKRI) Future Leaders Fellowship. Additional support for the laser calibration system and cosmic ray tagger was provided by the Albert Einstein Center for Fundamental Physics, Bern, Switzerland. We also acknowledge the contributions of technical and scientific sta↵to the design, construction, and operation of the MicroBooNE detector as well as the contributions of past collaborators to the development of MicroBooNE analyses, without whom this work would not have been possible. For the purpose of open access, the authors have applied a Creative Commons Attribution (CC BY) public copyright license to any Author Accepted Manuscript version arising from this submission. [1] Q. R. Ahmad et al. (SNO Collaboration), Measurement of the rate of ⌫e+d!p+p+einteractions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory, Phys. Rev. Lett. 87, 071301 (2001), arXiv:nuclex/0106015. [2] Y. Fukuda et al. (Super-Kamiokande Collaboration), Evidence for oscillation of atmospheric neutrinos, Phys. Rev. Lett. 81, 1562 (1998), arXiv:hep-ex/9807003. [3] B. Aharmim et al. (SNO Collaboration), Combined Analysis of all Three Phases of Solar Neutrino Data from the Sudbury Neutrino Observatory, Phys. Rev. C 88, 025501 (2013), arXiv:1109.0763 [nucl-ex]. Note: in 3+ 1 BOTH disappearance and appearance Antonio Palazzo, UNIBA & INFN 01/10/2025 18 5 surrounding material. Those neutrino interactions occur on heavier nuclei (e.g. iron, aluminium, lead) with larger cross section uncertainties (30%). This background is large at low energy. A control sample is used to measure the ⌫µN!⇡0X background. It is selected by requiring two electron-like tracks in the TPC with a common vertex in the FGD (distance between the starting points of the two tracks less than 10 mm) and invariant mass less than 50 MeV/c2. The control sample has an overall selection efficiency with respect to the total number of photons converting in the FGDs of about 12% and is a highly pure background sample predominantly consisting of photon conversion (92%) from ⌫µN!⇡0Xin NC and CCDIS interactions. The kinematics of the photons in the control and signal samples are similar. Furthermore, 62% of the control sample ⌫µevents are OOFV ⌫µN!⇡0X, which provides a direct constraint for the ⌫esample background. A more detailed description of the selection of both the ⌫eand the control samples is reported in [14]. The reconstructed ⌫eenergy spectrum (Ereco), assuming a CCQE interaction, is inferred from the outgoing electron candidate momentum and angle, as in [27]. ⌫e disappearance would a↵ect the rate and energy spectrum of ⌫eCC interactions. Fig. 3 shows the Ereco distributions of the ⌫eand the control samples. A total of 614 ⌫eCC candidates are selected in the ⌫esample and 665 ±51 (syst) events are expected, assuming no oscillation and with the systematic uncertainties described below. The number of selected events in the control sample is 989 in data, with an expectation of 1236 ±246 (syst). Systematic uncertainties on the flux, cross section and detector response are taken into account using the approach adopted in [14]. The systematic uncertainties on the flux and ⌫e-⌫µcommon cross sections are constrained by fitting the ⌫µCC sample as described earlier. The unconstrained cross-section systematic uncertainties include several contributions: the di↵erence between the interaction cross section of ⌫µand ⌫e,between⌫and ¯⌫ and the uncertainty on OOFV interactions. FSI uncertainties contribute 1.5% (2.7%) to the ⌫e(⌫µN!⇡0X) sample systematic uncertainty. The detector systematic uncertainties have been evaluated independently for the TPCs, FGDs and ECal. The largest sources of uncertainties are given by the TPC momentum resolution and the PID. In Table I, the e↵ect of each group of systematic uncertainties on the total expected number of signal and signal plus background events is shown. In Fig. 3 the e↵ect of the systematic uncertainties on the Ereco distributions is shown. The simulation overestimates the data in both the ⌫eand control sample distributions at low energy. However this overestimation in the control sample is within one standard deviation of expectation. Oscillation fit — The sterile oscillation parameters sin22✓ee and m2 e↵are estimated with a Poisson binned likelihood ratio method. The expected reconstructed neutrino energy distributions are compared to data with a simultaneous fit to the selected ⌫eand control samples. Events per bin 10 20 30 40 50 60 70 80 90 Data e ν X 0 π → N µ νIn-FV X 0 π →N µ νOOFV other µ ν Energy (GeV)νReconstructed 1 10 Data/MC 0.5 1 1.5 Events per bin 50 100 150 200 250 300 350 Data e ν X 0 π → N µ νIn-FV X 0 π →N µ νOOFV other µ ν Energy (GeV)νReconstructed 1 10 Data/MC 0.5 1 1.5 FIG. 3. Reconstructed energy distributions of the ⌫e(top) and control (bottom) samples. The distributions are broken down by ⌫einteractions (signal), background inside the fiducial volume due to ⌫µN!⇡0X(In-FV ⌫µN!⇡0X), background outside the fiducial volume due to ⌫µN!⇡0X (OOFV ⌫µN!⇡0X) and all other sources of background (⌫µother). Both ⌫and ¯⌫are included in the samples. The ratio of the data to the MC expectation in the null oscillation hypothesis is shown for both samples. The red error band corresponds to the fractional systematic uncertainty. Black dots represent the data with the statistical uncertainty. TABLE I. Fractional variation (RMS/mean in %) of the expected total number of events for ⌫e(all events and signal only) and control sample in the null oscillation hypothesis due to the e↵ect of the systematic uncertainties. Existing correlations between systematics are taken into account. Error source (# param.) ⌫esample ⌫esample control (sig+bkg) (sig only) sample ⌫µ-⌫ecommon (40) 4.4 5.2 6.7 Unconstrained (5) 3.7 3.0 17.8 Detector + FSI (10) 5.1 5.5 5.5 Total (55) 7.6 8.1 19.9 6 FIG. 4. The ratio of the best fit spectrum to the expected MC distribution, where the fit includes nuisance and oscillation parameters (blue) and nuisance parameters only (red dashed), is shown. The plots show the ⌫esample (top) and the control sample (bottom). The black line corresponds to the expected non-oscillated MC before the fit. The black dots show the data. Statistical uncertainties are shown. The range of Ereco is from 0.2 GeV to 10 GeV. The oscillation amplitude sin22✓ee is restricted to the physical region. The e↵ect of systematic uncertainties is included in the fit with nuisance parameters (55 in total) constrained by a Gaussian penalty term. The oscillation probability Eq. (1) a↵ects ⌫esignal events based on the true neutrino energy and flight path. The best-fit oscillation parameters are sin22✓ee = 1 and m2 e↵=2.05 eV2/c4.The2/ndf is 42.16/49. Most of the best-fit systematic parameters are within a 0.5deviations and always within 1from the prior values. The systematic parameter corresponding to the normalization of the ⌫µN!⇡0XOOFV component is reduced by 31% (⇠1) due to the deficit at low energy in the control sample. The ratio between the best-fit and the expected non-oscillated MC distributions is shown as a function of Ereco for both the ⌫eand the control samples in Fig. 4. The best-fit, where the nuisance parameters are allowed to float while the oscillation parameters are fixed to null, is also shown. The corresponding 2/ndf is 45.86/51. The two-dimensional confidence intervals in the sin22✓ee -m2 e↵parameter space are computed using ee θ 2 2 sin -1 10 1 ) 4 /c 2 (eV eff 2 mΔ -1 10 1 10 2 10 Allowed region at 68% CL Allowed region at 90% CL Excluded region at 95% CL FIG. 5. 68% and 90% CL allowed regions and 95% CL exclusion region for the sin22✓ee -m2 e↵parameters measured with the T2K near detector. the Feldman-Cousins method [28]. The systematic uncertainties are incorporated using the method described in [29]. The 68%, 90% and 95% confidence regions are shown in Fig. 5. The exclusion region at 95% CL is approximately given by sin22✓ee >0.3 and m2 e↵> 7eV 2/c4. The p-value of the null oscillation hypothesis, computed using a profile likelihood ratio as a test statistic, is 0.085. The impact of ⌫µdisappearance and ⌫eappearance on the present result is estimated by considering a nonnull sin22✓µµ in the 3+1 model. For sin22✓µµ between 0 and 0.05, approximately the region not excluded by other experiments [10, 30], the 95%CL exclusion on sin22✓ee moves by less than 0.1 In Fig. 6 the T2K excluded region at 95% CL is compared with ⌫edisappearance allowed regions from the gallium anomaly and reactor anomaly. The excluded regions from ⌫e+12 C!12N+escattering data of KARMEN [31, 32] and LSND [33] experiments and solar neutrino and KamLAND data [34–46] are also shown. The T2K result excludes part of the gallium anomaly and a small part of the reactor anomaly allowed regions. The current T2K limit at 95% CL is contained within the region excluded by the combined fit of the solar and KamLAND data. Conclusions — T2K has performed a search for ⌫edisappearance with the near detector. The excluded region at 95% CL is approximately sin22✓ee >0.3 and m2 e↵>7eV 2/c4. The p-value of the null oscillation hypothesis is 0.085. Further data from T2K will reduce the statistical uncertainty, which is still an important limitation for the analysis. Hint of nedisappearance in T2K T2K, arXiv: 1410.8811 [hep-ex] PRD 91, 051102 (21015) Note: ONLY disappearance (no app. considered) Antonio Palazzo, UNIBA & INFN New-Gen Reactor Experiments 1901/10/2025 Antonio Palazzo, UNIBA & INFN Universe 2021,7, 360 4 of 12 Table 1. Comparison of the experimental parameters (reactor thermal power Pth , water equivalent overburden D , baseline L , target mass m ), detection technique and statistical method used in the search for sterile neutrinos at reactors. If more than one detector site or method exists, a full list is given. Experiment Pth/MW D/m.w.e. L/m m/t Detection Method SoLid 80 10 6–9 1.6 6Li-PS n.a. NEOS 2800 20 24 1.0 Gd-LS RS DANSS 3100 50 11–13 0.9 Gd-LS CLs STEREO 58 15 9–11 1.7 Gd-LS RS, 2D, CLs PROSPECT 85 1 7–9 4.0 6Li-PS 2D, CLs Neutrino-4 100 5–10 6–12 1.5 Gd-LS 2D Daya Bay 17,400 250, 860 550, 1650 80, 80 Gd-LS 2D, CLs D-Chooz 8500 120, 300 400, 1050 8, 8 Gd-LS RS RENO 16,800 120, 450 294, 1383 16, 16 Gd-LS 2D, CLs Figure 1. Exclusion contours of all reactor experiments in the plane of ⇥sin2(2qee),Dm2 41⇤ alongside the allowed contours of the RAA and Gallium anomaly as well as Neutrino-4. KATRIN’s current and expected exclusion limits are shown in addition. Reprinted from [29] under CC BY 4.0. 2.1.1. SoLid The SoLid experiment [ 30 ] is located at baselines between 6 and 9m from the BR2 HEU reactor in Belgium. Its core has a height of 90cm and a diameter of 50 cm, providing 80MW thermal power. The detector, placed at an overburden of 10m.w.e., is foreseen to exploit a novel technique aiming for a high vertex resolution of the IBD event and a good neutron–gamma discrimination. The detector target has a composite scintillator design made from 16 ⇥ 16 cubes of 5cm width consisting of polyvinyl toluene (PVT) scintillator, which are optically separated by reflective Tyvek. Two faces of each PVT cube are covered by a layer of LiF:ZnS(Ag) to detect neutrons. The signal to background ratio in SoLid is estimated to be 0.33. No oscillation results have been reported by SoLid to date. Universe 2021,7, 360 4 of 12 Table 1. Comparison of the experimental parameters (reactor thermal power Pth , water equivalent overburden D , baseline L , target mass m ), detection technique and statistical method used in the search for sterile neutrinos at reactors. If more than one detector site or method exists, a full list is given. Experiment Pth/MW D/m.w.e. L/m m/t Detection Method SoLid 80 10 6–9 1.6 6Li-PS n.a. NEOS 2800 20 24 1.0 Gd-LS RS DANSS 3100 50 11–13 0.9 Gd-LS CLs STEREO 58 15 9–11 1.7 Gd-LS RS, 2D, CLs PROSPECT 85 1 7–9 4.0 6Li-PS 2D, CLs Neutrino-4 100 5–10 6–12 1.5 Gd-LS 2D Daya Bay 17,400 250, 860 550, 1650 80, 80 Gd-LS 2D, CLs D-Chooz 8500 120, 300 400, 1050 8, 8 Gd-LS RS RENO 16,800 120, 450 294, 1383 16, 16 Gd-LS 2D, CLs Figure 1. Exclusion contours of all reactor experiments in the plane of ⇥sin2(2qee),Dm2 41⇤ alongside the allowed contours of the RAA and Gallium anomaly as well as Neutrino-4. KATRIN’s current and expected exclusion limits are shown in addition. Reprinted from [29] under CC BY 4.0. 2.1.1. SoLid The SoLid experiment [ 30 ] is located at baselines between 6 and 9m from the BR2 HEU reactor in Belgium. Its core has a height of 90cm and a diameter of 50 cm, providing 80MW thermal power. The detector, placed at an overburden of 10m.w.e., is foreseen to exploit a novel technique aiming for a high vertex resolution of the IBD event and a good neutron–gamma discrimination. The detector target has a composite scintillator design made from 16 ⇥ 16 cubes of 5cm width consisting of polyvinyl toluene (PVT) scintillator, which are optically separated by reflective Tyvek. Two faces of each PVT cube are covered by a layer of LiF:ZnS(Ag) to detect neutrons. The signal to background ratio in SoLid is estimated to be 0.33. No oscillation results have been reported by SoLid to date. Universe 2021,7, 360 4 of 12 Table 1. Comparison of the experimental parameters (reactor thermal power Pth , water equivalent overburden D , baseline L , target mass m ), detection technique and statistical method used in the search for sterile neutrinos at reactors. If more than one detector site or method exists, a full list is given. Experiment Pth/MW D/m.w.e. L/m m/t Detection Method SoLid 80 10 6–9 1.6 6Li-PS n.a. NEOS 2800 20 24 1.0 Gd-LS RS DANSS 3100 50 11–13 0.9 Gd-LS CLs STEREO 58 15 9–11 1.7 Gd-LS RS, 2D, CLs PROSPECT 85 1 7–9 4.0 6Li-PS 2D, CLs Neutrino-4 100 5–10 6–12 1.5 Gd-LS 2D Daya Bay 17,400 250, 860 550, 1650 80, 80 Gd-LS 2D, CLs D-Chooz 8500 120, 300 400, 1050 8, 8 Gd-LS RS RENO 16,800 120, 450 294, 1383 16, 16 Gd-LS 2D, CLs Figure 1. Exclusion contours of all reactor experiments in the plane of ⇥sin2(2qee),Dm2 41⇤ alongside the allowed contours of the RAA and Gallium anomaly as well as Neutrino-4. KATRIN’s current and expected exclusion limits are shown in addition. Reprinted from [29] under CC BY 4.0. 2.1.1. SoLid The SoLid experiment [ 30 ] is located at baselines between 6 and 9m from the BR2 HEU reactor in Belgium. Its core has a height of 90cm and a diameter of 50cm, providing 80MW thermal power. The detector, placed at an overburden of 10m.w.e., is foreseen to exploit a novel technique aiming for a high vertex resolution of the IBD event and a good neutron–gamma discrimination. The detector target has a composite scintillator design made from 16 ⇥ 16 cubes of 5cm width consisting of polyvinyl toluene (PVT) scintillator, which are optically separated by reflective Tyvek. Two faces of each PVT cube are covered by a layer of LiF:ZnS(Ag) to detect neutrons. The signal to background ratio in SoLid is estimated to be 0.33. No oscillation results have been reported by SoLid to date. are probing increasingly large parameter space Schoppmann,arXiv: 2109.13541 [hep-ex] Universe 7 (2021) 10, 360 19 Tension among RAA and Gallium Anomaly Gariazzo et al. 2018 20 |Ue4|2 ∆m41 2 [eV2] 10−310−210−1 10−1 1 10 2−3σ (solid−dashed) Reactor Anomaly Gallium Anomaly NEOS+DANSS 1σ 2σ 3σ 10-310-210-1 10-1 100 101 |Ue4 2 m41 2[eV2] Gallium Solar SK+DC +IC C12 All edisapp All Reactors 95%, 99%CL 2 dof (a) (b) Figure 3 Results on SBL() ⌫edisappearance found in Ref. (84) (a) and Ref. (85) (b). The shaded regions in panel (a) have been obtained from the combined fit of the NEOS/Daya Bay and DANSS spectral ratio data (NEOS+DANSS). The blue and red contour lines delimit the regions allowed by the reactor and Gallium anomalies, respectively, at 2(solid lines) and 3(dashed lines). The blue shaded regions in panel (b) were obtained in Ref. (85) from a global fit of the reactor neutrino data including the NEOS/Daya Bay and DANSS spectral ratio data and the total event rates considering as free the dominant 235Uand239Pu reactor ¯⌫efluxes and constraining the subdominant 238Uand241Pu fluxes around their theoretical predictions with a large 10% uncertainty. The red shaded regions have been obtained by adding the Gallium, solar, and ⌫e-12C constraints, that are also shown separately. The figure shows also the atmospheric neutrino constraint obtained from the Super-Kamiokande (SK) (92), DeepCore (DC) (93) and IceCube (IC) (94) data, that is comparable to the solar neutrino constraint. flux calculations. Let us however emphasize that the model-independent indication hinges crucially on the NEOS/Daya Bay and DANSS spectral ratios that must be confirmed by new experiments. It is also important to emphasize that the search for SBL() ⌫edisappearance is of fundamental importance independently from the validity or not of the indication of() ⌫µ! () ⌫eappearance discussed in the following subsection, because it is possible that |Ue4|2' 0.01, whereas |Uµ4|2is much smaller and the corresponding() ⌫µ!() ⌫eappearance and () ⌫µ disappearance has not been seen yet. 4.2. ⌫µ!⌫eand ¯⌫µ!¯⌫eappearance Figure 4 illustrates the results of all the relevant SBL () ⌫µ!() ⌫eappearance experiments: LSND (4), MiniBooNE (6), BNL-E776 (96), KARMEN (5), NOMAD (97), ICARUS (98) and OPERA (99). Of all the experiments only LSND and MiniBooNE found indications in favor of SBL() ⌫µ!() ⌫etransitions and in Fig. 4a they have closed contours in the plane of the oscillation parameters sin22#eµ and m2 41. The other experiments provide exclusion curves that constitute upper limits on sin22#eµ for each value of m2 41. The di↵erence between Figs. 4a and 4b is that in Fig. 4a all the MiniBooNE data are used, whereas Fig. 4b the controversial low-energy MiniBooNE data are omitted according to the “pragmatic www.annualreviews.org •eV-scale Sterile Neutrinos 17 Dentler et al. 2018 01/10/2025 Antonio Palazzo, UNIBA & INFN Tension quoted at 2-3 sigma level 20 01/10/2025 21 unexplained n e appearance Antonio Palazzo, UNIBA & INFN The SBL accelerator anomalies LSND [LSND, PRL 75 (1995) 2650; PRC 54 (1996) 2685; PRL 77 (1996) 3082; PRD 64 (2001) 112007] ¯ ¯eL30 m 20 MeV E200 MeV other p(ν _ e,e+)n p(ν _ µ→ν _ e,e+)n L/Eν (meters/MeV) Beam Excess Beam Excess 0 2.5 5 7.5 10 12.5 15 17.5 0.4 0.6 0.8 1 1.2 1.4 10 -2 10 -1 1 10 10 2 10 -3 10 -2 10 -1 1 sin2 2θ Δm2 (eV2/c4) Bugey Karmen NOMAD CCFR 90% (Lmax-L < 2.3) 99% (Lmax-L < 4.6) ∆m2 LSND !02eV2(∆m2 ATM ∆m2 SOL) C. Giunti Phenomenology of Sterile Neutrinos 16 May 2011 5/59 LSND (unexplained neappearance in a nµbeam) MiniBooNE 01/10/2025 22 3 TABLE I: The expected (unconstrained) number of events for the 200 <E QE ⌫<1250 MeV neutrino energy range from all of the backgrounds in the ⌫eand ¯⌫eappearance analysis. Also shown are the constrained background and the expected number of events corresponding to the LSND best fit oscillation probability of 0.26%. The table shows the diagonal-element systematic uncertainties, which become substantially reduced in the oscillation fits when correlations between energy bins and between the electron and muon neutrino events are included. The antineutrino numbers are from a previous analysis [3]. Process Neutrino Mode Antineutrino Mode ⌫µ&¯⌫µCCQE 73.7 ±19.3 12.9 ±4.3 NC ⇡0501.5 ±65.4 112.3 ±11.5 NC !N172.5 ±24.1 34.7 ±5.4 External Events 75.2 ±10.9 15.3 ±2.8 Other ⌫µ&¯⌫µ89.6 ±22.9 22.3 ±3.5 ⌫e&¯⌫efrom µ±Decay 425.3 ±100.2 91.4 ±27.6 ⌫e&¯⌫efrom K±Decay 192.2 ±41.9 51.2 ±11.0 ⌫e&¯⌫efrom K0 LDecay 54.5 ±20.5 51.4 ±18.0 Other ⌫e&¯⌫e6.0 ±3.2 6.7 ±6.0 Unconstrained Bkgd. 1590.5 398.2 Constrained Bkgd. 1577.8±85.2398.7±28.6 Total Data 1959 478 Excess 381.2 ±85.2 79.3 ±28.6 0.26% (LSND) ⌫µ!⌫e463.1 100.0 energy range for the total 12.84 ⇥1020 POT data. Each bin of reconstructed EQE ⌫corresponds to a distribution of “true” generated neutrino energies, which can overlap adjacent bins. In neutrino mode, a total of 1959 data events pass the ⌫eCCQE event selection requirements with 200 <E QE ⌫<1250 MeV, compared to a background expectation of 1577.8±39.7(stat.)±75.4(syst.) events. The excess is then 381.2±85.2 events or a 4.5e↵ect. Note that the 162.0 event excess in the first 6.46 ⇥1020 POT data is approximately 1lower than the average excess, while the 219.2 event excess in the second 6.38 ⇥1020 POT data is approximately 1 higher than the average excess. Combining the MiniBooNE neutrino and antineutrino data, there are a total of 2437 events in the 200 <E QE ⌫<1250 MeV energy region, compared to a background expectation of 1976.5±44.5(stat.)±84.8(syst.) events. This corresponds to a total ⌫eplus ¯⌫eCCQE excess of 460.5±95.8events with respect to expectation or a 4.8excess. The significance of the combined LSND (3.8) [1] and MiniBooNE (4.8)excessesis6.1. Fig. 2 shows the total event excesses as a function of EQE ⌫in both neutrino mode and antineutrino mode. The dashed curves show the best fits to standard two-neutrino oscillations. Fig. 3 compares the L/EQE ⌫distributions for the MiniBooNE data excesses in neutrino mode and antineutrino mode to the L/E distribution from LSND [1]. The error bars show statistical uncertainties only. As shown in the figure, there is agreement among all three data sets. Fitting these data to standard two-neutrino oscillations including statistical errors only, the best fit oc0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 (GeV) QE ν E 0 1 2 3 4 5 Events/MeV Data (stat err.) +/- µ from e ν+/- from K e ν0 from K e ν misid 0 π γ N→ Δ dirt other Constr. Syst. Error Best Fit 3.0 FIG. 1: The MiniBooNE neutrino mode EQE ⌫distributions, corresponding to the total 12.84 ⇥1020 POT data, for ⌫e CCQE data (points with statistical errors) and background (histogram with systematic errors). The dashed curve shows the best fit to the neutrino-mode data assuming standard twoneutrino oscillations. FIG. 2: The MiniBooNE total event excesses as a function of EQE ⌫in both neutrino mode and antineutrino mode, corresponding to 12.84 ⇥1020 POT and 11.27 ⇥1020 POT, respectively. (Error bars include both statistical and correlated systematic uncertainties.) The dashed curves show the best fits to the neutrino-mode and antineutrino-mode data assuming standard two-neutrino oscillations. curs at m2=0.040 eV2and sin22✓=0.894 with a2/ndf = 35.2/28, corresponding to a probability of 16.4%. This best fit agrees with the MiniBooNE only best fit described below. The MiniBooNE excess of events in both oscillation probability and L/E spectrum is, therefore, consistent with the LSND excess of events, even though the two experiments have completely different neutrino energies, neutrino fluxes, reconstruction, backgrounds, and systematic uncertainties. 4 FIG. 3: A comparison between the L/EQE ⌫distributions for the MiniBooNE data excesses in neutrino mode (12.84 ⇥1020 POT) and antineutrino mode (11.27⇥1020 POT) to the L/E distribution from LSND [1]. The error bars show statistical uncertainties only. The solid curve shows the best fit to the LSND and MiniBooNE data assuming standard two-neutrino oscillations. The excess of MiniBooNE electron-neutrino candidate events is consistent with the LSND excess. A standard two-neutrino model is assumed for the MiniBooNE oscillation fits. Note, however, that there are tensions with fits presented here between appearance and disappearance experiments [10, 12], and other models [15–19] may provide better fits to the data. The oscillation parameters are extracted from a combined fit of the observed EQE ⌫event distributions for muon-like and electron-like events using the full covariance matrix described previously. The fit assumes the same oscillation probability for both the right-sign ⌫eand wrong-sign ¯⌫e, and no significant ⌫µ,¯⌫µ,⌫e, or ¯⌫edisappearance. Using a likelihood-ratio technique [3], the confidence level values for the fitting statistic, 2=2(point)2(best), as a function of oscillation parameters, m2and sin22✓, is determined from frequentist, fake data studies. With this technique, the best neutrino oscillation fit in neutrino mode for 200 <E QE ⌫<1250 MeV occurs at (m2, sin22✓) = (0.037 eV2, 0.958), as shown in Fig. 4. The 2/ndf is 10.0/6.6 with a probability of 15.4%. The background-only fit has a 2-probability of 0.02% relative to the best oscillation fit and a 2/ndf = 26.7/8.8witha probability of 0.14%. Fig. 4 shows the MiniBooNE closed confidence level (CL) contours for ⌫eappearance oscillations in neutrino mode in the 200 <E QE ⌫<1250 MeV energy range. Nuclear e↵ects associated with neutrino interactions on carbon can a↵ect the reconstruction of the neutrino energy, EQE ⌫, and the determination of the neutrino oscillation parameters [33]. These e↵ects were studied previously [3] and were found to not a↵ect substantially the oscillation fit. In addition, they do not a↵ect the gamma 3− 10 2− 10 1− 10 1 θ2 2 sin 2− 10 1− 10 1 10 2 10 ) 2 (eV 2 mΔ 90% CL KARMEN2 90% CL OPERA LSND 90% CL LSND 99% CL 68% CL 90% CL 95% CL 99% CL CLσ3 CLσ4 FIG. 4: MiniBooNE allowed regions in neutrino mode (12.84⇥ 1020 POT) for events with 200 <E QE ⌫<1250 MeV within a two-neutrino oscillation model. The shaded areas show the 90% and 99% C.L. LSND ¯⌫µ!¯⌫eallowed regions. The black circle shows the MiniBooNE best fit point. Also shown are 90% C.L. limits from the KARMEN [34] and OPERA [35] experiments. background, which is determined from direct measurements of NC ⇡0and dirt backgrounds. Fig. 5 shows the MiniBooNE allowed regions in both neutrino mode and antineutrino mode [3] for events with 200 <E QE ⌫<1250 MeV within a two-neutrino oscillation model. For this oscillation fit the entire data set is used and includes the 12.84 ⇥1020 POT in neutrino mode and the 11.27⇥1020 POT in antineutrino mode. As shown in the figure, the MiniBooNE favored allowed region overlaps with the LSND allowed region. Also shown are 90% C.L. limits from the KARMEN [34] and OPERA [35] experiments. The best combined neutrino oscillation fit occurs at (m2,sin 22✓) = (0.041 eV2, 0.958). The 2/ndf for the best-fit point is 19.5/15.4 with a probability of 20.1%, and the background-only fit has a 2probability of 5 ⇥107relative to the best oscillation fit and a 2/ndf = 49.3/17.5 with a probability of 0.007%. Fitting both LSND and MiniBooNE data, the best fit remains at (m2,sin 22✓) = (0.041 eV2, 0.958) with a 2/ndf = 22.4/23.4, corresponding to a probability of 52.0%. In summary, the MiniBooNE experiment observes a total ⌫eCCQE event excess in both neutrino and an3.8s 4.8s 22Antonio Palazzo, UNIBA & INFN Appearance-Disapparance tension in 3+1 fits 23 Dentler et al arXiv:1803.10661 JHEP 08 (2018) 010 01/10/2025 Antonio Palazzo, UNIBA & INFN Tension quoted at 4-5 sigma level in different independent analyses 19 10-410-310-210-1 10-1 100 101 sin22e m2[eV2] Disappearance Free Fluxes Fixed Fluxes Appearance (w/o DiF) 99.73%CL 2 dof FIG. 7. Appearance versus disappearance data in the plane spanned by the e↵ective mixing angle sin22✓µe ⌘4|Ue4Uµ4|2and the mass squared di↵erence m2 41. The blue curves show limits from the disappearance data sets using free reactor fluxes (solid) or fixed reactor fluxes (dashed), while the shaded contours are based on the appearance data sets using LSND DaR+DiF (red) and LSND DaR (pink hatched). All contours are at 99.73% CL for 2 dof. two additional free parameters. We would now like to quantify the tension between di↵erent subsets of the global data that is evident from fig. 5. We first note that combining all data sets we find a goodness-of-fit for the global best fit point around 65%, see table VI.Thisgoodp-value does not reflect the tension we found because many data points entering the global fit have only little sensitivity to sterile neutrino oscillations, thus diluting the power of a goodness-of-fit test based on 2/dof. A more reliable method for quantifying the compatibility of di↵erentdatasetsisthe parameter goodness-of-fit (PG) test [92], which measures the penalty in 2that one has to pay for combining data sets, see appendix Afor a brief review of this test. If the global neutrino oscillation data were consistent when interpreted in the framework of a 3 + 1 model, any slicing into two statistically independent data sets Aand Bshould result in an acceptable p-value from the PG test. To illustrate an inconsistency in the data, it is however sufficient to demonstrate that at least one way of dividing it leads to a poor value. Here, we choose to split the data into disappearance data encompassing the oscillation channels (–) ⌫e!(–) ⌫eand (–) ⌫µ!(–) ⌫µ, and appearance data covering the (–) ⌫µ!(–) ⌫echannel. Note that it is important to chose data sets independent of their “result”. For instance, dividing data into “evidence” and “no-evidence” samples would bias the PG test. The tension between appearance and disappearance data is shown graphically in fig. 7. The figure illustrates the lack of overlap between the parameter region favoured by appearance data (driven by LSND and MiniBooNE) and the strong exclusion limits from disappearance data. The tension persists independently of whether reactor fluxes are fixed or kept free, and whether the LSND DaR or DaR+DiF samples are used. The corresponding results from the PG test are shown in the last two columns of table VI.Toevaluatethe 23 01/10/2025 24 nµdisappearance Antonio Palazzo, UNIBA & INFN 01/10/2025 25 6 3− 10 2− 10 1− 10 1 24 θ 2 sin 4− 10 3− 10 2− 10 1− 10 1 10 2 10 3 10 ) 2 (eV 41 2 mΔ MINOS/MINOS+ Excluded FC 90% C.L. )σ and 2σSensitivity FC 90% C.L. (median, 1 S Excluded 90% CL Figure 2. Comparison of the MINOS and MINOS+ 90% C.L. exclusion contour using the Feldman-Cousins method [52] and the CLs method. The regions to the right of the curves are excluded at the 90% C.L. (CLs). The 90% C.L. median sensitivity is shown in red along with the 1and 2bands. ders of magnitude in the sterile mass-squared splitting m2 41. These limits are the world’s most stringent over 5 orders of magnitude, for m2 41 .10 eV2. The new constraints exclude the entire 90% C.L. allowed regions from LSND and MiniBooNE for m2 41 <5eV2, with regions at higher values being excluded by NOMAD [54]. Further, the 99% C.L. allowed regions from LSND and MiniBooNE are excluded for m2 41 <1.2eV2. The allowed region from a global fit to data from sterile neutrino probes, intentionally excluding MINOS, MINOS+, Daya Bay, and Bugey-3 contributions, computed by the authors of Refs. [55, 56], is fully excluded at the 99% C.L. The allowed region resulting from a fit to all appearance data, updated by the authors of Ref. [57] to include the MiniBooNE 2018 results [21], is equally strongly excluded. The new limits presented here thus significantly increase the tension between pure sterile neutrino mixing explanations of appearance-based indications and the null results from disappearance searches. The sole consideration of additional sterile neutrino states cannot resolve this tension, which stems from the non-observation of ¯⌫eand() ⌫µdisappearance beyond what is expected from the three-neutrino mixing model. This inconsistency may be further quantified in additional detector exposures in the process of being analyzed, specifically the last year of MINOS+ data taking, representing an additional sample of similar size to the one used here, as well as over two more years of Daya Bay data. Figure 3. Comparison of the MINOS, MINOS+, Daya Bay, and Bugey-3 combined 90% CLslimit on sin22✓µe to the LSND and MiniBooNE 90% C.L. allowed regions. Regions of parameter space to the right of the red contour are excluded. The regions excluded at 90% C.L. by the KARMEN2 Collaboration [53] and the NOMAD Collaboration [54] are also shown. The combined limit also excludes the 90% C.L. region allowed by a fit to global data by Gariazzo et al. where MINOS, MINOS+, Daya Bay, and Bugey-3 are not included [55, 56], and the 90% C.L. region allowed by a fit to all available appearance data by Dentler et al. [57] updated with the 2018 MiniBooNE appearance results [21]. We gratefully acknowledge valuable contributions by Carlo Giunti, for supplying a custom fit to global data excluding MINOS, MINOS+, Daya Bay, and Bugey-3 data, and by Mona Dentler and Joachim Kopp, for providing an updated version of a fit to global appearance data including information from the 2018 MiniBooNE appearance results. The Daya Bay experiment is supported in part by the Ministry of Science and Technology of China, the U.S. Department of Energy, the Chinese Academy of Sciences, the CAS Center for Excellence in Particle Physics, the National Natural Science Foundation of China, the Guangdong provincial government, the Shenzhen municipal government, the China General Nuclear Power Group, the Research Grants Council of the Hong Kong Special Administrative Region of China, the Ministry of Education in Taiwan, the U.S. National Science Foundation, the Ministry of Education, Youth and Sports of the Czech Republic, the Joint Institute of Nuclear Research in Dubna, Russia, the NSFC-RFBR joint research program, and the National Commission for Scientific and Technological Research of Chile. We acknowledge Yellow River Engineering Consulting Co., Ltd. and China Railway 15th Bureau Group Co., Ltd. for building the underground laboratory. We are grateful for the ongoing cooperation from the China MINOS/MINOS+ arXiv: 2002.00301 [hep-ex] PRL 125, 071801 (2020) 6 4− 10 3− 10 2− 10 1− 10 1 24 θ 2 sin 3− 10 2− 10 1− 10 1 10 2 10 ) 2 (eV 2 41 mΔ -beamν 90% CL excluded NOvA Analysis 1 NOvA Analysis 2 MINOS/MINOS+ CDHS CCFR T2K (NH) T2K (IH) SciBooNE & MiniBooNE Super-Kamiokande 90% CL allowed IceCube 90% CL allowed IceCube (a) 2− 10 1− 10 1 34 θ 2 sin 3− 10 2− 10 1− 10 1 10 2 10 ) 2 (eV 2 41 mΔ -beamν 90% CL excluded NOvA Analysis 1 NOvA Analysis 2 Super-Kamiokande IceCube-DeepCore MINOS T2K (b) (c) FIG. 3: NOvA’s Feldman–Cousins corrected 90 % confidence limits in (a) m2 41 sin2✓24 space, (b) m2 41 sin2✓34 space, and (c) m2 41 sin22✓µ⌧space with allowed regions and exclusion contours from other experiments [21–33, 62]. Regions to the right of open contours are excluded. Closed contours for SciBooNE/MiniBooNE, CCFR, and CDHS in (a) also denote exclusion regions. For Super-Kamiokande, a single value of each mixing angle is reported for m2 41 0.1eV 2[26]. Arrows in (b) represent a constraint on sin2✓34 at a single value of m2 41 [24, 27, 33]. OPERA NH/IH contours in (c) overlap at m2 41 >102eV2. comes from muon neutrino disappearance, which is independent of ✓34 (Eq. 2). For high values of m2 41 sensitivity is driven by the ND data, meaning di↵erences in the limits come from di↵erent handling of the systematic uncertainties. Sensitivity at low m2 41 arises primarily from FD data, meaning that the weaker limit in Analysis 2 comes from under-coverage of the CNP statistical technique. Our m2 41sin2✓34 contours (Fig. 3b) represent worldleading limits for m2 41 <0.1eV 2. Sensitivity to sin 2✓34 comes from our NC samples. For oscillations at the sterile frequency, oscillation probability /cos2✓34 sin2✓24, resulting in reduced sensitivity to sterile oscillations in the ND (Eq. 1). For this space our sensitivity comes primarily from oscillations at the atmospheric frequency and therefore FD data, which are statistically limited and without strong dependence on m2 41. In this space, Analysis 1 excludes slightly more parameter space than Analysis 2 across the full range considered. The di↵erences in the contours in this space are attributed to the di↵erent statistical treatments of the two analyses. Finally, in Fig. 3c, we present our results in terms of the e↵ective mixing parameter, sin22✓µ⌧=4|Uµ4|2|U⌧4|2= sin2✓24 sin2✓34, which can be thought of as describing anomalous sterile-driven ⌫⌧appearance. Because the analyses are consistent and the Feldman–Cousins procedure is resource intensive, we choose to present this contour using only Analysis 1. NOvA’s ND is at a higher L/E⌫than other experiments with limits in this space, meaning that we are able to probe to lower values of m2 41 resulting in the NOvA 90 % limit being worldleading across large areas below m2 41 =3eV 2. Notably, this limit excludes a new region of phase space around m2 41 =1eV 2, the preferred region of m2 41 for current anomalies. In conclusion, an improved search for sterile neutrino oscillations under the 3+1 oscillation paradigm has been performed using NOvA data. We use two covariance matrix-based techniques that allow us to probe a wider range of m2 41 values than previous NOvA analyses [43, 44]. Di↵erences between the limits for the two analyses can be taken as an uncertainty due to analysis choices such as statistical treatment, systematic treatment, binning of the 2surface, and fitting technique. We find that the NOvA data are consistent with 3F oscillations at 90 % confidence, and our limits agree with sensitivity studies performed using 3F oscillations. Our limits are the first presented in some regions of phase space, while excluding new regions of parameter space currently allowed by IceCube at 90 % confidence level. This work additionally sets the most stringent limits for anomalous ⌫⌧appearance for m2 41 .3eV 2, including the strongest limits around m2 41 =1eV 2. This document was prepared by the NOvA collaboration using the resources of the Fermi National Accelerator Laboratory (Fermilab), a U.S. Department of Energy, NOvA arXiv: 2409.04553 [hep-ex] PRL 134, 081804 (2025) No nµdisappearance in SBL/LBL Figure 48. The MINOS and MINOS+ 90% Feldman-Cousins exclusion limit compared to the previous MINOS result [299] and results from other experiments. The Gariazzo et al. region is the result of a global fit to neutrino oscillation data [300]. Figure from [142]. data looking for electron (anti)neutrino disappearance, as described in Sec. 4.1.3.4 NOvA The NuMI O↵-Axis ⌫eAppearance (NOvA) experiment is a long-baseline accelerator neutrino experiment based at Fermilab and the Far Detector Laboratory at Ash River, Minnesota. NOvA has as its primary goal to measure three-neutrino mixing parameters, including the determination of the neutrino mass ordering, by looking for the appearance of electron neutrinos or antineutrinos, and the disappearance of muon neutrinos or antineutrinos, using the NuMI neutrino beam produced at Fermilab. This is accomplished by using two detectors separated by 810 km, placed 14 mrad o↵the NuMI beam axis. Due to the o↵-axis placement, the detectors sample a narrow range of neutrino energies between 1 and 4 GeV, peaking at 2 GeV as shown in Fig. 49. This configuration is chosen to drastically reduce the feed-down of NC interactions of higher-energy neutrinos, which typically represent the dominant background to the measurement of ⌫eCC interactions in on-axis experiments. The 0.33 kton ND is located underground next to the MINOS ND hall at Fermilab, while the 14 kton FD is positioned at the surface in Ash River, Minnesota. Both detectors are composed of extruded 32-cell PVC modules filled with liquid scintillators. The cells are read out by 32-pixel avalanche photodiodes (APDs). NOvA began collecting data in 2014 and has so far accumulated large samples in both neutrino-dominated and antineutrino-dominated modes. NOvA placed constraints on sterile neutrinos via searches for di↵erences in the rate of NC neutrino interactions between the Near and Far detectors. The analysis was based on 6.05 ⇥1020 protons-on-target taken in neutrino-dominated mode, and 95 NC candidates were selected at the Far Detector compared with 83.5±9.7(stat.)±9.4(syst.)eventspredicted assuming mixing only occurs between active neutrino species. Therefore, NOvA found no 79 Antonio Palazzo, UNIBA & INFN CCFR and CDHS SciBooNE+MiniBooNE 01/10/2025 NO n Aprefers d CP ∼ 0.9 p Bird’s-eye view: 2024 T2K prefers d CP ∼ 1.5 p { <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> June 17, 2024 / NEUTRINO '24 J. Wolcott / Tufts U. 36 Far detector observations: νe Data favors region where matter & CP violation e/ects oppose one another Future ν data will be critical for disentangling ν ν Oscillation analysis results •Preference for δCP~-π/2 but CP conserving values are within the 2σ interval 18 Sample δCP=-π/2 δCP=0 δCP=π/2 δCP=πData 𝜈-mode 1Rμ417.2 416.3 417.1 418.2 357 𝜈-mode MR 123.9 123.3 123.9 124.4 140 𝜈-mode 1Rμ146.6 146.3 146.6 147.0 137 𝜈-mode 1Re 113.2 95.5 78.3 96.0 102 𝜈-mode 1Re+d.e. 10.0 8.8 7.2 8.4 15 𝜈-mode 1Re 17.6 20.0 22.2 19.7 16 Credible intervals marginalized over both hierarchies D. Carabadjac poster 0 20 40 60 80 100 120 140 Neutrino mode e-like candidates 8 10 12 14 16 18 20 22 24 26 Antineutrino mode e-like candidates 11 Preliminary−T2K Run1 0.60, 0.55, 0.50, 0.45 = 23 θ 2 sin 2 eV 3− 10× = 2.52 32 2 m∆ 2 eV 3− 10×2.49− = 31 2 m∆ π = CP δ /2π+ = CP δ = 0 CP δ /2π− = CP δ 68% syst err. at best-fit Best-fit Data (68% stat err.) δCP Δχ2 for Nomal Ordering: TENSION PERSISTING T2K almost unaltered statistics NOvA doubled n statistics Almost unchanged Antonio Palazzo, UNIBA & INFN 32 0.0 0.5 1.0 1.5 2.0 0 5 10 15 20 dCPêp Dc2 T2K NOvA T2K+NOvA c2 DcT2K 2 DcNOvA 2 cmin 2 01/10/2025 Quantification of tension ¯2(CP)=2 T2K+NOvA(CP)(2 T2K,min +2 NOvA,min) <latexit 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sha1_base64="EH4e6or0GzibfMCTXU6ZFVnTl6I=">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</latexit> Maltoni & Schwetz Criterion hep-ph/0304176 PRD (2003) ¯2 min =6.3 <latexit 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sha1_base64="B+5JYQ0+ybLLsMAFhi9j+sWWhU0=">AAACAXicbVDLSsNAFJ34rPUVdSO4GSyCq5BUUTdC0Y3LCvYBTQyT6aQdOjMJMxOhhLrxV9y4UMStf+HOv3HaZqGtBy4czrmXe++JUkaVdt1va2FxaXlltbRWXt/Y3Nq2d3abKskkJg2csES2I6QIo4I0NNWMtFNJEI8YaUWD67HfeiBS0UTc6WFKAo56gsYUI22k0N6HfoSkj/v0vhrmnIoRvIRnzkk5tCuu404A54lXkAooUA/tL7+b4IwToTFDSnU8N9VBjqSmmJFR2c8USREeoB7pGCoQJyrIJx+M4JFRujBOpCmh4UT9PZEjrtSQR6aTI91Xs95Y/M/rZDq+CHIq0kwTgaeL4oxBncBxHLBLJcGaDQ1BWFJzK8R9JBHWJrRxCN7sy/OkWXU81/FuTyu1qyKOEjgAh+AYeOAc1MANqIMGwOARPINX8GY9WS/Wu/UxbV2wipk98AfW5w/KDZUl</latexit> <latexit sha1_base64="B+5JYQ0+ybLLsMAFhi9j+sWWhU0=">AAACAXicbVDLSsNAFJ34rPUVdSO4GSyCq5BUUTdC0Y3LCvYBTQyT6aQdOjMJMxOhhLrxV9y4UMStf+HOv3HaZqGtBy4czrmXe++JUkaVdt1va2FxaXlltbRWXt/Y3Nq2d3abKskkJg2csES2I6QIo4I0NNWMtFNJEI8YaUWD67HfeiBS0UTc6WFKAo56gsYUI22k0N6HfoSkj/v0vhrmnIoRvIRnzkk5tCuu404A54lXkAooUA/tL7+b4IwToTFDSnU8N9VBjqSmmJFR2c8USREeoB7pGCoQJyrIJx+M4JFRujBOpCmh4UT9PZEjrtSQR6aTI91Xs95Y/M/rZDq+CHIq0kwTgaeL4oxBncBxHLBLJcGaDQ1BWFJzK8R9JBHWJrRxCN7sy/OkWXU81/FuTyu1qyKOEjgAh+AYeOAc1MANqIMGwOARPINX8GY9WS/Wu/UxbV2wipk98AfW5w/KDZUl</latexit> GoF = 1.4⇥102 <latexit 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sha1_base64="KBA7BgFMMnwcUkg5NWfp5bVOh+8=">AAACB3icbVDLSsNAFJ34rPUVdSnIYBHcGJJS0I1QFNRlBfuAJpbJdNIOnWTCzEQoITs3/oobF4q49Rfc+TdO2iy09cCFwzn3cu89fsyoVLb9bSwsLi2vrJbWyusbm1vb5s5uS/JEYNLEnHHR8ZEkjEakqahipBMLgkKfkbY/usz99gMRkvLoTo1j4oVoENGAYqS01DMPXBGm1/wqg+fQsWrQVTQkEjr2fXpSzco9s2Jb9gRwnjgFqYACjZ755fY5TkISKcyQlF3HjpWXIqEoZiQru4kkMcIjNCBdTSOkt3np5I8MHmmlDwMudEUKTtTfEykKpRyHvu4MkRrKWS8X//O6iQrOvJRGcaJIhKeLgoRBxWEeCuxTQbBiY00QFlTfCvEQCYSVji4PwZl9eZ60qpZjW85trVK/KOIogX1wCI6BA05BHdyABmgCDB7BM3gFb8aT8WK8Gx/T1gWjmNkDf2B8/gA3uZb0</latexit> <latexit sha1_base64="KBA7BgFMMnwcUkg5NWfp5bVOh+8=">AAACB3icbVDLSsNAFJ34rPUVdSnIYBHcGJJS0I1QFNRlBfuAJpbJdNIOnWTCzEQoITs3/oobF4q49Rfc+TdO2iy09cCFwzn3cu89fsyoVLb9bSwsLi2vrJbWyusbm1vb5s5uS/JEYNLEnHHR8ZEkjEakqahipBMLgkKfkbY/usz99gMRkvLoTo1j4oVoENGAYqS01DMPXBGm1/wqg+fQsWrQVTQkEjr2fXpSzco9s2Jb9gRwnjgFqYACjZ755fY5TkISKcyQlF3HjpWXIqEoZiQru4kkMcIjNCBdTSOkt3np5I8MHmmlDwMudEUKTtTfEykKpRyHvu4MkRrKWS8X//O6iQrOvJRGcaJIhKeLgoRBxWEeCuxTQbBiY00QFlTfCvEQCYSVji4PwZl9eZ60qpZjW85trVK/KOIogX1wCI6BA05BHdyABmgCDB7BM3gFb8aT8WK8Gx/T1gWjmNkDf2B8/gA3uZb0</latexit> <latexit sha1_base64="KBA7BgFMMnwcUkg5NWfp5bVOh+8=">AAACB3icbVDLSsNAFJ34rPUVdSnIYBHcGJJS0I1QFNRlBfuAJpbJdNIOnWTCzEQoITs3/oobF4q49Rfc+TdO2iy09cCFwzn3cu89fsyoVLb9bSwsLi2vrJbWyusbm1vb5s5uS/JEYNLEnHHR8ZEkjEakqahipBMLgkKfkbY/usz99gMRkvLoTo1j4oVoENGAYqS01DMPXBGm1/wqg+fQsWrQVTQkEjr2fXpSzco9s2Jb9gRwnjgFqYACjZ755fY5TkISKcyQlF3HjpWXIqEoZiQru4kkMcIjNCBdTSOkt3np5I8MHmmlDwMudEUKTtTfEykKpRyHvu4MkRrKWS8X//O6iQrOvJRGcaJIhKeLgoRBxWEeCuxTQbBiY00QFlTfCvEQCYSVji4PwZl9eZ60qpZjW85trVK/KOIogX1wCI6BA05BHdyABmgCDB7BM3gFb8aT8WK8Gx/T1gWjmNkDf2B8/gA3uZb0</latexit> Antonio Palazzo, UNIBA & INFN 33 Chatterjee & Palazzo arXiv:2409.10599 PRD 11 113002 (2024) 01/10/2025 T2K and NOvA have different baselines and peak energies (L/E = costant) Why to consider non-standard interactions Matter effects depend on the ratio v=2VCCE m2 31 =0.18 E 2.0 GeV  <latexit 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sha1_base64="m1f1SRIfzE/OAUiYR8LYO6CRzz8=">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</latexit> v⇠0.05 <latexit 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sha1_base64="CI9WSwEwGQ5IGSeGaUVrRpLwNfs=">AAAB8nicbVDLSgMxFL1TX7W+qi7dBIvgqsyIosuiG5cV7AOmQ8mkmTY0jyHJFMrQz3DjQhG3fo07/8a0nYVWD4QczrmXe++JU86M9f0vr7S2vrG5Vd6u7Ozu7R9UD4/aRmWa0BZRXOlujA3lTNKWZZbTbqopFjGnnXh8N/c7E6oNU/LRTlMaCTyULGEEWyeFE9QzTCC/7l/1qzX3LYD+kqAgNSjQ7Fc/ewNFMkGlJRwbEwZ+aqMca8sIp7NKLzM0xWSMhzR0VGJBTZQvVp6hM6cMUKK0e9KihfqzI8fCmKmIXaXAdmRWvbn4nxdmNrmJcibTzFJJloOSjCOr0Px+NGCaEsunjmCimdsVkRHWmFiXUsWFEKye/Je0L+qBXw8eLmuN2yKOMpzAKZxDANfQgHtoQgsIKHiCF3j1rPfsvXnvy9KSV/Qcwy94H99tYZAG</latexit> T2K NOvA New matter effects encoded by NSI are also proportional to T2K is a “quasivacuum” experiment. Its estimate of dCP is independent of NSI. NOvA is a “matter dominated” experiment. The extracted value of dCP is affected by NSI. If NSI are taken into account, the estimate of dCP should return in agreement with that of T2K. Basic Idea: suppose NSI exist, then: v <latexit sha1_base64="Y1VFGg6QQHrr//k/0PvW2lPMVyo=">AAAB6HicbVBNS8NAEJ3Ur1q/qh69LBbBU0lE0GPRi8cW7Ae0oWy2k3btZhN2N4US+gu8eFDEqz/Jm//GbZuDtj4YeLw3w8y8IBFcG9f9dgobm1vbO8Xd0t7+weFR+fikpeNUMWyyWMSqE1CNgktsGm4EdhKFNAoEtoPx/dxvT1BpHstHM03Qj+hQ8pAzaqzUmPTLFbfqLkDWiZeTCuSo98tfvUHM0gilYYJq3fXcxPgZVYYzgbNSL9WYUDamQ+xaKmmE2s8Wh87IhVUGJIyVLWnIQv09kdFI62kU2M6ImpFe9ebif143NeGtn3GZpAYlWy4KU0FMTOZfkwFXyIyYWkKZ4vZWwkZUUWZsNiUbgrf68jppXVU9t+o1riu1uzyOIpzBOVyCBzdQgweoQxMYIDzDK7w5T86L8+58LFsLTj5zCn/gfP4A4zGM+g==</latexit> <latexit 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sha1_base64="s0RlfKeIBl3A5bQTzq1tXNmPsA4=">AAAB8nicbVDLSgNBEOyNrxhfUY9eBoPgKeyKEI9BLx4jmBjYLGF2MpsMmccyMxsISz7DiwdFvPo13vwbJ8keNLGgoajqprsrTjkz1ve/vdLG5tb2Tnm3srd/cHhUPT7pGJVpQttEcaW7MTaUM0nblllOu6mmWMScPsXju7n/NKHaMCUf7TSlkcBDyRJGsHVSOEE9wwTy60GjX635dX8BtE6CgtSgQKtf/eoNFMkElZZwbEwY+KmNcqwtI5zOKr3M0BSTMR7S0FGJBTVRvjh5hi6cMkCJ0q6kRQv190SOhTFTEbtOge3IrHpz8T8vzGxyE+VMppmlkiwXJRlHVqH5/2jANCWWTx3BRDN3KyIjrDGxLqWKCyFYfXmddK7qgYvs4brWvC3iKMMZnMMlBNCAJtxDC9pAQMEzvMKbZ70X7937WLaWvGLmFP7A+/wBce6QCQ==</latexit> <latexit sha1_base64="s0RlfKeIBl3A5bQTzq1tXNmPsA4=">AAAB8nicbVDLSgNBEOyNrxhfUY9eBoPgKeyKEI9BLx4jmBjYLGF2MpsMmccyMxsISz7DiwdFvPo13vwbJ8keNLGgoajqprsrTjkz1ve/vdLG5tb2Tnm3srd/cHhUPT7pGJVpQttEcaW7MTaUM0nblllOu6mmWMScPsXju7n/NKHaMCUf7TSlkcBDyRJGsHVSOEE9wwTy60GjX635dX8BtE6CgtSgQKtf/eoNFMkElZZwbEwY+KmNcqwtI5zOKr3M0BSTMR7S0FGJBTVRvjh5hi6cMkCJ0q6kRQv190SOhTFTEbtOge3IrHpz8T8vzGxyE+VMppmlkiwXJRlHVqH5/2jANCWWTx3BRDN3KyIjrDGxLqWKCyFYfXmddK7qgYvs4brWvC3iKMMZnMMlBNCAJtxDC9pAQMEzvMKbZ70X7937WLaWvGLmFP7A+/wBce6QCQ==</latexit> Antonio Palazzo, UNIBA & INFN 34 Chatterjee and Palazzo, arXiv: 2008:0416, PRL 126 051801 (2021) 01/10/2025 NSI substantially reduce the tension 0.0 0.5 1.0 1.5 2.0 0 5 10 15 20 dCPêp Dc2 SM+NSIH∂etL T2K NOvA T2K+NOvA 0.0 0.5 1.0 1.5 2.0 0 5 10 15 20 dCPêp Dc2 SM+NSIH∂emL T2K NOvA T2K+NOvA Antonio Palazzo, UNIBA & INFN 35 Single Dc 2obtained for the best fit of T2K + NO n A: ["eµ =0.13,eµ =1.35⇡] <latexit 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sha1_base64="4t8VLpyj98ybPuj6cY2R2eetgaY=">AAACHnicbZDLSgMxFIYz9VbrbdSlm2ARXJRhxlp0IxTduKxgLzAzlEx62oZmLiSZQhn6JG58FTcuFBFc6duYXkBt/SHw5zvnkJw/SDiTyra/jNzK6tr6Rn6zsLW9s7tn7h80ZJwKCnUa81i0AiKBswjqiikOrUQACQMOzWBwM6k3hyAki6N7NUrAD0kvYl1GidKobVZcb0gEJJJxfc3AC9MxvsK25ZRLXgl7SZ/9UMcqVzRiftss2pY9FV42ztwU0Vy1tvnhdWKahhApyomUrmMnys+IUIxyGBe8VEJC6ID0wNU2IiFIP5uuN8YnmnRwNxb6RApP6e+JjIRSjsJAd4ZE9eVibQL/q7mp6l76GYuSVEFEZw91U45VjCdZ4Q4TQBUfaUOoYPqvmPaJIFTpRAs6BGdx5WXTOLMcnebdebF6PY8jj47QMTpFDrpAVXSLaqiOKHpAT+gFvRqPxrPxZrzPWnPGfOYQ/ZHx+Q3D/aBR</latexit> ["e⌧=0.22,e⌧=1.70⇡] <latexit 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sha1_base64="RGT0cdYSd8IcQfZ69OUxJN8jzpk=">AAACIHicbZDLSgMxFIYz9VbrbdSlm2ARXJRhpgh1IxTduKxgL9AZSiY904ZmLiSZQhn6KG58FTcuFNGdPo1pO4va+kPgz3fOITm/n3AmlW1/G4WNza3tneJuaW//4PDIPD5pyTgVFJo05rHo+EQCZxE0FVMcOokAEvoc2v7oblZvj0FIFkePapKAF5JBxAJGidKoZ9a67pgISCTj+pqBq0g6xTfYtqrVilvBbjJkS9ixarZmzOuZZduy58LrxslNGeVq9Mwvtx/TNIRIUU6k7Dp2oryMCMUoh2nJTSUkhI7IALraRiQE6WXzBaf4QpM+DmKhT6TwnC5PZCSUchL6ujMkaihXazP4X62bquDay1iUpAoiungoSDlWMZ6lhftMAFV8og2hgum/YjokglClMy3pEJzVlddNq2o5tuU8XJXrt3kcRXSGztElclAN1dE9aqAmougJvaA39G48G6/Gh/G5aC0Y+cwp+iPj5xdyI6E0</latexit> <latexit sha1_base64="RGT0cdYSd8IcQfZ69OUxJN8jzpk=">AAACIHicbZDLSgMxFIYz9VbrbdSlm2ARXJRhpgh1IxTduKxgL9AZSiY904ZmLiSZQhn6KG58FTcuFNGdPo1pO4va+kPgz3fOITm/n3AmlW1/G4WNza3tneJuaW//4PDIPD5pyTgVFJo05rHo+EQCZxE0FVMcOokAEvoc2v7oblZvj0FIFkePapKAF5JBxAJGidKoZ9a67pgISCTj+pqBq0g6xTfYtqrVilvBbjJkS9ixarZmzOuZZduy58LrxslNGeVq9Mwvtx/TNIRIUU6k7Dp2oryMCMUoh2nJTSUkhI7IALraRiQE6WXzBaf4QpM+DmKhT6TwnC5PZCSUchL6ujMkaihXazP4X62bquDay1iUpAoiungoSDlWMZ6lhftMAFV8og2hgum/YjokglClMy3pEJzVlddNq2o5tuU8XJXrt3kcRXSGztElclAN1dE9aqAmougJvaA39G48G6/Gh/G5aC0Y+cwp+iPj5xdyI6E0</latexit> ["e⌧= 0] <latexit 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sha1_base64="UrIuBlf2KTpOVaU106h0/gyzQeM=">AAACAnicbVDLSsNAFJ3UV62vqCtxM1gEVyURQTdC0Y3LCvYBSSiT6U07dDIJM5NCCcWNv+LGhSJu/Qp3/o3TNgttPXDhzDn3MveeMOVMacf5tkorq2vrG+XNytb2zu6evX/QUkkmKTRpwhPZCYkCzgQ0NdMcOqkEEocc2uHwduq3RyAVS8SDHqcQxKQvWMQo0Ubq2keePyISUsW4eebga5JN8DV2gq5ddWrODHiZuAWpogKNrv3l9xKaxSA05UQpz3VSHeREakY5TCp+piAldEj64BkqSAwqyGcnTPCpUXo4SqQpofFM/T2Rk1ipcRyazpjogVr0puJ/npfp6CrImUgzDYLOP4oyjnWCp3ngHpNANR8bQqhkZldMB0QSqk1qFROCu3jyMmmd11yn5t5fVOs3RRxldIxO0Bly0SWqozvUQE1E0SN6Rq/ozXqyXqx362PeWrKKmUP0B9bnD9nVlws=</latexit> ["eµ = 0] <latexit 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sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> { <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit 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sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> 01/10/2025 T2K regions almost unaltered NO n A regions strongly modified NSI bring the estimates of d CP in agreement 68% & 90% CL 2 dof Antonio Palazzo, UNIBA & INFN 36 ["eµ =0.13,eµ =1.35⇡] <latexit sha1_base64="4t8VLpyj98ybPuj6cY2R2eetgaY=">AAACHnicbZDLSgMxFIYz9VbrbdSlm2ARXJRhxlp0IxTduKxgLzAzlEx62oZmLiSZQhn6JG58FTcuFBFc6duYXkBt/SHw5zvnkJw/SDiTyra/jNzK6tr6Rn6zsLW9s7tn7h80ZJwKCnUa81i0AiKBswjqiikOrUQACQMOzWBwM6k3hyAki6N7NUrAD0kvYl1GidKobVZcb0gEJJJxfc3AC9MxvsK25ZRLXgl7SZ/9UMcqVzRiftss2pY9FV42ztwU0Vy1tvnhdWKahhApyomUrmMnys+IUIxyGBe8VEJC6ID0wNU2IiFIP5uuN8YnmnRwNxb6RApP6e+JjIRSjsJAd4ZE9eVibQL/q7mp6l76GYuSVEFEZw91U45VjCdZ4Q4TQBUfaUOoYPqvmPaJIFTpRAs6BGdx5WXTOLMcnebdebF6PY8jj47QMTpFDrpAVXSLaqiOKHpAT+gFvRqPxrPxZrzPWnPGfOYQ/ZHx+Q3D/aBR</latexit> <latexit sha1_base64="4t8VLpyj98ybPuj6cY2R2eetgaY=">AAACHnicbZDLSgMxFIYz9VbrbdSlm2ARXJRhxlp0IxTduKxgLzAzlEx62oZmLiSZQhn6JG58FTcuFBFc6duYXkBt/SHw5zvnkJw/SDiTyra/jNzK6tr6Rn6zsLW9s7tn7h80ZJwKCnUa81i0AiKBswjqiikOrUQACQMOzWBwM6k3hyAki6N7NUrAD0kvYl1GidKobVZcb0gEJJJxfc3AC9MxvsK25ZRLXgl7SZ/9UMcqVzRiftss2pY9FV42ztwU0Vy1tvnhdWKahhApyomUrmMnys+IUIxyGBe8VEJC6ID0wNU2IiFIP5uuN8YnmnRwNxb6RApP6e+JjIRSjsJAd4ZE9eVibQL/q7mp6l76GYuSVEFEZw91U45VjCdZ4Q4TQBUfaUOoYPqvmPaJIFTpRAs6BGdx5WXTOLMcnebdebF6PY8jj47QMTpFDrpAVXSLaqiOKHpAT+gFvRqPxrPxZrzPWnPGfOYQ/ZHx+Q3D/aBR</latexit> <latexit sha1_base64="4t8VLpyj98ybPuj6cY2R2eetgaY=">AAACHnicbZDLSgMxFIYz9VbrbdSlm2ARXJRhxlp0IxTduKxgLzAzlEx62oZmLiSZQhn6JG58FTcuFBFc6duYXkBt/SHw5zvnkJw/SDiTyra/jNzK6tr6Rn6zsLW9s7tn7h80ZJwKCnUa81i0AiKBswjqiikOrUQACQMOzWBwM6k3hyAki6N7NUrAD0kvYl1GidKobVZcb0gEJJJxfc3AC9MxvsK25ZRLXgl7SZ/9UMcqVzRiftss2pY9FV42ztwU0Vy1tvnhdWKahhApyomUrmMnys+IUIxyGBe8VEJC6ID0wNU2IiFIP5uuN8YnmnRwNxb6RApP6e+JjIRSjsJAd4ZE9eVibQL/q7mp6l76GYuSVEFEZw91U45VjCdZ4Q4TQBUfaUOoYPqvmPaJIFTpRAs6BGdx5WXTOLMcnebdebF6PY8jj47QMTpFDrpAVXSLaqiOKHpAT+gFvRqPxrPxZrzPWnPGfOYQ/ZHx+Q3D/aBR</latexit> <latexit sha1_base64="4t8VLpyj98ybPuj6cY2R2eetgaY=">AAACHnicbZDLSgMxFIYz9VbrbdSlm2ARXJRhxlp0IxTduKxgLzAzlEx62oZmLiSZQhn6JG58FTcuFBFc6duYXkBt/SHw5zvnkJw/SDiTyra/jNzK6tr6Rn6zsLW9s7tn7h80ZJwKCnUa81i0AiKBswjqiikOrUQACQMOzWBwM6k3hyAki6N7NUrAD0kvYl1GidKobVZcb0gEJJJxfc3AC9MxvsK25ZRLXgl7SZ/9UMcqVzRiftss2pY9FV42ztwU0Vy1tvnhdWKahhApyomUrmMnys+IUIxyGBe8VEJC6ID0wNU2IiFIP5uuN8YnmnRwNxb6RApP6e+JjIRSjsJAd4ZE9eVibQL/q7mp6l76GYuSVEFEZw91U45VjCdZ4Q4TQBUfaUOoYPqvmPaJIFTpRAs6BGdx5WXTOLMcnebdebF6PY8jj47QMTpFDrpAVXSLaqiOKHpAT+gFvRqPxrPxZrzPWnPGfOYQ/ZHx+Q3D/aBR</latexit> See also Denton, Gehrlein & Pestes, PRL 126 051801 (2021) 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09 0.1 0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.02 0.03 0.04 0.05 0.06 0.07 0.08 0.09 0.1 0.01 0.02 0.03 0.04 0.05 0.06 0.07 01/10/2025 In agreement with dCP ∼3p/2 ellipse. On this ellipse it pins down feµ ∼3p/2 Strongly favors dCP ∼3p/2 ellipse (almost no sensitivity to feµ) ……. dCP = 0 ……. dCP = p/2 ……. dCP = p ****** dCP = 3p/2 ▲ feµ= 0 ◼ feµ= p/2 ● feµ= p ◆ feµ= 3p/2 NO n A T2K Pµe <latexit sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> <latexit 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sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> Pµe <latexit sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> <latexit sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> <latexit sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> <latexit sha1_base64="ciw3O1Yuy3iAvYzySy5qkTQJLH8=">AAAB8HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48RzEOSJcxOOsmQmdllZlYIS77CiwdFvPo53vwbJ8keNLGgoajqprsrSgQ31ve/vcLa+sbmVnG7tLO7t39QPjxqmjjVDBssFrFuR9Sg4AoblluB7UQjlZHAVjS+nfmtJ9SGx+rBThIMJR0qPuCMWic91ntZV6YEp71yxa/6c5BVEuSkAjnqvfJXtx+zVKKyTFBjOoGf2DCj2nImcFrqpgYTysZ0iB1HFZVowmx+8JScOaVPBrF2pSyZq78nMiqNmcjIdUpqR2bZm4n/eZ3UDq7DjKsktajYYtEgFcTGZPY96XONzIqJI5Rp7m4lbEQ1ZdZlVHIhBMsvr5LmRTXwq8H9ZaV2k8dRhBM4hXMI4ApqcAd1aAADCc/wCm+e9l68d+9j0Vrw8plj+APv8weSMpA+</latexit> ¯ Pµe <latexit sha1_base64="ks8qJue0si6V7vedpAmbjtWPkaQ=">AAAB9XicbVBNS8NAEJ34WetX1aOXxSJ4KokIeix68VjBfkATy2Y7aZduNmF3o5TQ/+HFgyJe/S/e/Ddu2xy09cHA470ZZuaFqeDauO63s7K6tr6xWdoqb+/s7u1XDg5bOskUwyZLRKI6IdUouMSm4UZgJ1VI41BgOxzdTP32IyrNE3lvxikGMR1IHnFGjZUe/JAq0ujlfpwRnPQqVbfmzkCWiVeQKhRo9Cpffj9hWYzSMEG17npuaoKcKsOZwEnZzzSmlI3oALuWShqjDvLZ1RNyapU+iRJlSxoyU39P5DTWehyHtjOmZqgXvan4n9fNTHQV5FymmUHJ5ouiTBCTkGkEpM8VMiPGllCmuL2VsCFVlBkbVNmG4C2+vExa5zXPrXl3F9X6dRFHCY7hBM7Ag0uowy00oAkMFDzDK7w5T86L8+58zFtXnGLmCP7A+fwB7n6SIQ==</latexit> <latexit sha1_base64="ks8qJue0si6V7vedpAmbjtWPkaQ=">AAAB9XicbVBNS8NAEJ34WetX1aOXxSJ4KokIeix68VjBfkATy2Y7aZduNmF3o5TQ/+HFgyJe/S/e/Ddu2xy09cHA470ZZuaFqeDauO63s7K6tr6xWdoqb+/s7u1XDg5bOskUwyZLRKI6IdUouMSm4UZgJ1VI41BgOxzdTP32IyrNE3lvxikGMR1IHnFGjZUe/JAq0ujlfpwRnPQqVbfmzkCWiVeQKhRo9Cpffj9hWYzSMEG17npuaoKcKsOZwEnZzzSmlI3oALuWShqjDvLZ1RNyapU+iRJlSxoyU39P5DTWehyHtjOmZqgXvan4n9fNTHQV5FymmUHJ5ouiTBCTkGkEpM8VMiPGllCmuL2VsCFVlBkbVNmG4C2+vExa5zXPrXl3F9X6dRFHCY7hBM7Ag0uowy00oAkMFDzDK7w5T86L8+58zFtXnGLmCP7A+fwB7n6SIQ==</latexit> <latexit sha1_base64="ks8qJue0si6V7vedpAmbjtWPkaQ=">AAAB9XicbVBNS8NAEJ34WetX1aOXxSJ4KokIeix68VjBfkATy2Y7aZduNmF3o5TQ/+HFgyJe/S/e/Ddu2xy09cHA470ZZuaFqeDauO63s7K6tr6xWdoqb+/s7u1XDg5bOskUwyZLRKI6IdUouMSm4UZgJ1VI41BgOxzdTP32IyrNE3lvxikGMR1IHnFGjZUe/JAq0ujlfpwRnPQqVbfmzkCWiVeQKhRo9Cpffj9hWYzSMEG17npuaoKcKsOZwEnZzzSmlI3oALuWShqjDvLZ1RNyapU+iRJlSxoyU39P5DTWehyHtjOmZqgXvan4n9fNTHQV5FymmUHJ5ouiTBCTkGkEpM8VMiPGllCmuL2VsCFVlBkbVNmG4C2+vExa5zXPrXl3F9X6dRFHCY7hBM7Ag0uowy00oAkMFDzDK7w5T86L8+58zFtXnGLmCP7A+fwB7n6SIQ==</latexit> <latexit sha1_base64="ks8qJue0si6V7vedpAmbjtWPkaQ=">AAAB9XicbVBNS8NAEJ34WetX1aOXxSJ4KokIeix68VjBfkATy2Y7aZduNmF3o5TQ/+HFgyJe/S/e/Ddu2xy09cHA470ZZuaFqeDauO63s7K6tr6xWdoqb+/s7u1XDg5bOskUwyZLRKI6IdUouMSm4UZgJ1VI41BgOxzdTP32IyrNE3lvxikGMR1IHnFGjZUe/JAq0ujlfpwRnPQqVbfmzkCWiVeQKhRo9Cpffj9hWYzSMEG17npuaoKcKsOZwEnZzzSmlI3oALuWShqjDvLZ1RNyapU+iRJlSxoyU39P5DTWehyHtjOmZqgXvan4n9fNTHQV5FymmUHJ5ouiTBCTkGkEpM8VMiPGllCmuL2VsCFVlBkbVNmG4C2+vExa5zXPrXl3F9X6dRFHCY7hBM7Ag0uowy00oAkMFDzDK7w5T86L8+58zFtXnGLmCP7A+fwB7n6SIQ==</latexit> |"eµ|=0.15 <latexit sha1_base64="SoKhE+IURXHckVI95i3jNNqomXo=">AAACBHicbVDLSsNAFJ34rPUVddnNYBFclUQU3QhFNy4r2Ac0oUymN+3QySTMTAol7cKNv+LGhSJu/Qh3/o3TNgttPXDhzDn3MveeIOFMacf5tlZW19Y3Ngtbxe2d3b19++CwoeJUUqjTmMeyFRAFnAmoa6Y5tBIJJAo4NIPB7dRvDkEqFosHPUrAj0hPsJBRoo3UsUtjb0gkJIpx88zAi9LJGF9jp+JedOyyU3FmwMvEzUkZ5ah17C+vG9M0AqEpJ0q1XSfRfkakZpTDpOilChJCB6QHbUMFiUD52eyICT4xSheHsTQlNJ6pvycyEik1igLTGRHdV4veVPzPa6c6vPIzJpJUg6Dzj8KUYx3jaSK4yyRQzUeGECqZ2RXTPpGEapNb0YTgLp68TBpnFddEdn9ert7kcRRQCR2jU+SiS1RFd6iG6oiiR/SMXtGb9WS9WO/Wx7x1xcpnjtAfWJ8/3pyXiw==</latexit> <latexit sha1_base64="SoKhE+IURXHckVI95i3jNNqomXo=">AAACBHicbVDLSsNAFJ34rPUVddnNYBFclUQU3QhFNy4r2Ac0oUymN+3QySTMTAol7cKNv+LGhSJu/Qh3/o3TNgttPXDhzDn3MveeIOFMacf5tlZW19Y3Ngtbxe2d3b19++CwoeJUUqjTmMeyFRAFnAmoa6Y5tBIJJAo4NIPB7dRvDkEqFosHPUrAj0hPsJBRoo3UsUtjb0gkJIpx88zAi9LJGF9jp+JedOyyU3FmwMvEzUkZ5ah17C+vG9M0AqEpJ0q1XSfRfkakZpTDpOilChJCB6QHbUMFiUD52eyICT4xSheHsTQlNJ6pvycyEik1igLTGRHdV4veVPzPa6c6vPIzJpJUg6Dzj8KUYx3jaSK4yyRQzUeGECqZ2RXTPpGEapNb0YTgLp68TBpnFddEdn9ert7kcRRQCR2jU+SiS1RFd6iG6oiiR/SMXtGb9WS9WO/Wx7x1xcpnjtAfWJ8/3pyXiw==</latexit> <latexit sha1_base64="SoKhE+IURXHckVI95i3jNNqomXo=">AAACBHicbVDLSsNAFJ34rPUVddnNYBFclUQU3QhFNy4r2Ac0oUymN+3QySTMTAol7cKNv+LGhSJu/Qh3/o3TNgttPXDhzDn3MveeIOFMacf5tlZW19Y3Ngtbxe2d3b19++CwoeJUUqjTmMeyFRAFnAmoa6Y5tBIJJAo4NIPB7dRvDkEqFosHPUrAj0hPsJBRoo3UsUtjb0gkJIpx88zAi9LJGF9jp+JedOyyU3FmwMvEzUkZ5ah17C+vG9M0AqEpJ0q1XSfRfkakZpTDpOilChJCB6QHbUMFiUD52eyICT4xSheHsTQlNJ6pvycyEik1igLTGRHdV4veVPzPa6c6vPIzJpJUg6Dzj8KUYx3jaSK4yyRQzUeGECqZ2RXTPpGEapNb0YTgLp68TBpnFddEdn9ert7kcRRQCR2jU+SiS1RFd6iG6oiiR/SMXtGb9WS9WO/Wx7x1xcpnjtAfWJ8/3pyXiw==</latexit> <latexit sha1_base64="SoKhE+IURXHckVI95i3jNNqomXo=">AAACBHicbVDLSsNAFJ34rPUVddnNYBFclUQU3QhFNy4r2Ac0oUymN+3QySTMTAol7cKNv+LGhSJu/Qh3/o3TNgttPXDhzDn3MveeIOFMacf5tlZW19Y3Ngtbxe2d3b19++CwoeJUUqjTmMeyFRAFnAmoa6Y5tBIJJAo4NIPB7dRvDkEqFosHPUrAj0hPsJBRoo3UsUtjb0gkJIpx88zAi9LJGF9jp+JedOyyU3FmwMvEzUkZ5ah17C+vG9M0AqEpJ0q1XSfRfkakZpTDpOilChJCB6QHbUMFiUD52eyICT4xSheHsTQlNJ6pvycyEik1igLTGRHdV4veVPzPa6c6vPIzJpJUg6Dzj8KUYx3jaSK4yyRQzUeGECqZ2RXTPpGEapNb0YTgLp68TBpnFddEdn9ert7kcRRQCR2jU+SiS1RFd6iG6oiiR/SMXtGb9WS9WO/Wx7x1xcpnjtAfWJ8/3pyXiw==</latexit> The Matter-Vacuum Synergy Use T2K as an anchor for NOvA Antonio Palazzo, UNIBA & INFN 37 0.0 0.5 1.0 1.5 2.0 0 5 10 15 dCPêp Dc2 SM, NO SM, IO 0.0 0.5 1.0 1.5 2.0 0 5 10 15 dCPêp Dc2 eem, NO eem, IO 01/10/2025 3-flavor NSI restore the preference for NO 3-flavor + NSI Better agreement with all the other data T2K + NO n AT2K + NO n A Antonio Palazzo, UNIBA & INFN 38 0.0 0.5 1.0 1.5 2.0 0 5 10 15 dCPêp Dc2 SM, NO SM, IO 01/10/2025 Can the tension be resolved assuming IO? For IO the best fit of d CP is the same in T2K and NOvA (left panel). However, IO gains only c 2IO - c 2NO ∼- 1 in T2K + NOvA combination (middle panel). The reason is that T2K disfavors IO (dotted ellipses) (right panel). T2K and NO n Adisappearance channel + Reactors prefer NO ( c 2IO - c 2NO ∼ 3). SK atmospheric data prefer NO ( c 2IO - c 2NO ∼ 6). T2K + NO n A Therefore, IO seems not to be the favored solution but I think it is still premature do discard it Oscillation analysis results •Preference for δCP~-π/2 but CP conserving values are within the 2σ interval 18 Sample δCP=-π/2 δCP=0 δCP=π/2 δCP=πData 𝜈-mode 1Rμ417.2 416.3 417.1 418.2 357 𝜈-mode MR 123.9 123.3 123.9 124.4 140 𝜈-mode 1Rμ146.6 146.3 146.6 147.0 137 𝜈-mode 1Re 113.2 95.5 78.3 96.0 102 𝜈-mode 1Re+d.e. 10.0 8.8 7.2 8.4 15 𝜈-mode 1Re 17.6 20.0 22.2 19.7 16 Credible intervals marginalized over both hierarchies D. Carabadjac poster 0 20 40 60 80 100 120 140 Neutrino mode e-like candidates 8 10 12 14 16 18 20 22 24 26 Antineutrino mode e-like candidates 11 Preliminary−T2K Run1 0.60, 0.55, 0.50, 0.45 = 23 θ 2 sin 2 eV 3− 10× = 2.52 32 2 m∆ 2 eV 3− 10×2.49− = 31 2 m∆ π = CP δ /2π+ = CP δ = 0 CP δ /2π− = CP δ 68% syst err. at best-fit Best-fit Data (68% stat err.) δCP Δχ2 Antonio Palazzo, UNIBA & INFN 39 01/10/2025 Antonio Palazzo, UNIBA & INFN 40 A more general and pedagogical analysis: [ e ee, e e µ ] In both NMO preferred large negative e ee ≃ -1 e ee in NO - e ee -2in IO As expected fittedat the same C.L. (degenerate) NO Note: for e ee = -1 NO and IO bievents ellipses coincide! Coloma& Schwetz 1604.05772 PRD 94 055005 (2016) IO 01/10/2025 Antonio Palazzo, UNIBA & INFN 41 FIG. 2: Isolines of !Pee"with standard MSW effects (aMSW=1) and with no matter effect (aMSW = 0). The gray region is allowed by the SK+SNO combination. No such region exist in the absence of MSW effects. 10 e ee = 0 e ee = -1 Solar MSW effects zeroed for e ee = -1 Fogli et al., hep-ph/0309100, PLB 583, 149 (2004) Pee > 0.5 Pee = 0.3 100 150 200 250 300 10 20 30 40 50 neApp. Events neApp. Events SM, NO ∂em, NO Data ¯ ‡ NOnA Ê 50 70 90 110 130 10 15 20 25 30 neApp. Events neApp. Events SM, NO ∂em, NO Data Ê ¯ ‡ T2K 48 Bievents plots in the presence of NSI 01/10/2025 Antonio Palazzo, UNIBA & INFN 48 ? <latexit sha1_base64="GE8gaIWQQKrHRkDMuP8w0LcyVSQ=">AAAB7HicbVBNS8NAEJ3Ur1q/qh69LBbBU0lEqMeiF48VTFtoQ9lsN+3SzSbsToQS+hu8eFDEqz/Im//GbZuDtj4YeLw3w8y8MJXCoOt+O6WNza3tnfJuZW//4PCoenzSNkmmGfdZIhPdDanhUijuo0DJu6nmNA4l74STu7nfeeLaiEQ94jTlQUxHSkSCUbSS3zdI9aBac+vuAmSdeAWpQYHWoPrVHyYsi7lCJqkxPc9NMcipRsEkn1X6meEpZRM64j1LFY25CfLFsTNyYZUhiRJtSyFZqL8nchobM41D2xlTHJtVby7+5/UyjG6CXKg0Q67YclGUSYIJmX9OhkJzhnJqCWVa2FsJG1NNGdp8KjYEb/XlddK+qntu3Xu4rjVvizjKcAbncAkeNKAJ99ACHxgIeIZXeHOU8+K8Ox/L1pJTzJzCHzifP/GMjsI=</latexit> <latexit 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sha1_base64="Yl9ebo2efGU1r9v7Lck9R9Ylz1I=">AAACAHicbVDLSsNAFJ3UV62vqAsXbgaL4KokIuiy6MZlBfuAJpTJ5LYdOpnEmYlQQjb+ihsXirj1M9z5N07TLLT1wMDhnPuaEyScKe0431ZlZXVtfaO6Wdva3tnds/cPOipOJYU2jXksewFRwJmAtmaaQy+RQKKAQzeY3Mz87iNIxWJxr6cJ+BEZCTZklGgjDewjr5iRSQhzL+CETtRDSiQM7LrTcArgZeKWpI5KtAb2lxfGNI1AaMqJUn3XSbSfEakZ5ZDXvFRBYsaTEfQNFSQC5WfF8hyfGiXEw1iaJzQu1N8dGYmUmkaBqYyIHqtFbyb+5/VTPbzyMyaSVIOg80XDlGMd41kaOGQSqOZTQwiVzNyK6ZhIQrXJrGZCcBe/vEw65w3Xabh3F/XmdRlHFR2jE3SGXHSJmugWtVAbUZSjZ/SK3qwn68V6tz7mpRWr7DlEf2B9/gDLLpcp</latexit> <latexit sha1_base64="Yl9ebo2efGU1r9v7Lck9R9Ylz1I=">AAACAHicbVDLSsNAFJ3UV62vqAsXbgaL4KokIuiy6MZlBfuAJpTJ5LYdOpnEmYlQQjb+ihsXirj1M9z5N07TLLT1wMDhnPuaEyScKe0431ZlZXVtfaO6Wdva3tnds/cPOipOJYU2jXksewFRwJmAtmaaQy+RQKKAQzeY3Mz87iNIxWJxr6cJ+BEZCTZklGgjDewjr5iRSQhzL+CETtRDSiQM7LrTcArgZeKWpI5KtAb2lxfGNI1AaMqJUn3XSbSfEakZ5ZDXvFRBYsaTEfQNFSQC5WfF8hyfGiXEw1iaJzQu1N8dGYmUmkaBqYyIHqtFbyb+5/VTPbzyMyaSVIOg80XDlGMd41kaOGQSqOZTQwiVzNyK6ZhIQrXJrGZCcBe/vEw65w3Xabh3F/XmdRlHFR2jE3SGXHSJmugWtVAbUZSjZ/SK3qwn68V6tz7mpRWr7DlEf2B9/gDLLpcp</latexit> <latexit sha1_base64="Yl9ebo2efGU1r9v7Lck9R9Ylz1I=">AAACAHicbVDLSsNAFJ3UV62vqAsXbgaL4KokIuiy6MZlBfuAJpTJ5LYdOpnEmYlQQjb+ihsXirj1M9z5N07TLLT1wMDhnPuaEyScKe0431ZlZXVtfaO6Wdva3tnds/cPOipOJYU2jXksewFRwJmAtmaaQy+RQKKAQzeY3Mz87iNIxWJxr6cJ+BEZCTZklGgjDewjr5iRSQhzL+CETtRDSiQM7LrTcArgZeKWpI5KtAb2lxfGNI1AaMqJUn3XSbSfEakZ5ZDXvFRBYsaTEfQNFSQC5WfF8hyfGiXEw1iaJzQu1N8dGYmUmkaBqYyIHqtFbyb+5/VTPbzyMyaSVIOg80XDlGMd41kaOGQSqOZTQwiVzNyK6ZhIQrXJrGZCcBe/vEw65w3Xabh3F/XmdRlHFR2jE3SGXHSJmugWtVAbUZSjZ/SK3qwn68V6tz7mpRWr7DlEf2B9/gDLLpcp</latexit> Best fit of [dCP, feµ, eeµ] of combination of T2K +NOVA CP =1.1⇡ <latexit sha1_base64="xlcIXPhYVz9nvFVg7brdqKKKocI=">AAACCHicbVDLSsNAFJ3UV62vqEsXDhbBVUhE0I1Q7MZlBfuAJoTJZNIOnUnCzEQoIUs3/oobF4q49RPc+TdO2iy09cCFwzn3cu89QcqoVLb9bdRWVtfWN+qbja3tnd09c/+gJ5NMYNLFCUvEIECSMBqTrqKKkUEqCOIBI/1g0i79/gMRkibxvZqmxONoFNOIYqS05JvHbkiYQn7ucqTGgsO83SkKeA0dy4FuSn2zaVv2DHCZOBVpggod3/xywwRnnMQKMyTl0LFT5eVIKIoZKRpuJkmK8ASNyFDTGHEivXz2SAFPtRLCKBG6YgVn6u+JHHEppzzQneW5ctErxf+8YaaiKy+ncZopEuP5oihjUCWwTAWGVBCs2FQThAXVt0I8RgJhpbNr6BCcxZeXSe/ccmzLubtotm6qOOrgCJyAM+CAS9ACt6ADugCDR/AMXsGb8WS8GO/Gx7y1ZlQzh+APjM8f4VKYkA==</latexit> <latexit sha1_base64="xlcIXPhYVz9nvFVg7brdqKKKocI=">AAACCHicbVDLSsNAFJ3UV62vqEsXDhbBVUhE0I1Q7MZlBfuAJoTJZNIOnUnCzEQoIUs3/oobF4q49RPc+TdO2iy09cCFwzn3cu89QcqoVLb9bdRWVtfWN+qbja3tnd09c/+gJ5NMYNLFCUvEIECSMBqTrqKKkUEqCOIBI/1g0i79/gMRkibxvZqmxONoFNOIYqS05JvHbkiYQn7ucqTGgsO83SkKeA0dy4FuSn2zaVv2DHCZOBVpggod3/xywwRnnMQKMyTl0LFT5eVIKIoZKRpuJkmK8ASNyFDTGHEivXz2SAFPtRLCKBG6YgVn6u+JHHEppzzQneW5ctErxf+8YaaiKy+ncZopEuP5oihjUCWwTAWGVBCs2FQThAXVt0I8RgJhpbNr6BCcxZeXSe/ccmzLubtotm6qOOrgCJyAM+CAS9ACt6ADugCDR/AMXsGb8WS8GO/Gx7y1ZlQzh+APjM8f4VKYkA==</latexit> <latexit sha1_base64="xlcIXPhYVz9nvFVg7brdqKKKocI=">AAACCHicbVDLSsNAFJ3UV62vqEsXDhbBVUhE0I1Q7MZlBfuAJoTJZNIOnUnCzEQoIUs3/oobF4q49RPc+TdO2iy09cCFwzn3cu89QcqoVLb9bdRWVtfWN+qbja3tnd09c/+gJ5NMYNLFCUvEIECSMBqTrqKKkUEqCOIBI/1g0i79/gMRkibxvZqmxONoFNOIYqS05JvHbkiYQn7ucqTGgsO83SkKeA0dy4FuSn2zaVv2DHCZOBVpggod3/xywwRnnMQKMyTl0LFT5eVIKIoZKRpuJkmK8ASNyFDTGHEivXz2SAFPtRLCKBG6YgVn6u+JHHEppzzQneW5ctErxf+8YaaiKy+ncZopEuP5oihjUCWwTAWGVBCs2FQThAXVt0I8RgJhpbNr6BCcxZeXSe/ccmzLubtotm6qOOrgCJyAM+CAS9ACt6ADugCDR/AMXsGb8WS8GO/Gx7y1ZlQzh+APjM8f4VKYkA==</latexit> <latexit sha1_base64="xlcIXPhYVz9nvFVg7brdqKKKocI=">AAACCHicbVDLSsNAFJ3UV62vqEsXDhbBVUhE0I1Q7MZlBfuAJoTJZNIOnUnCzEQoIUs3/oobF4q49RPc+TdO2iy09cCFwzn3cu89QcqoVLb9bdRWVtfWN+qbja3tnd09c/+gJ5NMYNLFCUvEIECSMBqTrqKKkUEqCOIBI/1g0i79/gMRkibxvZqmxONoFNOIYqS05JvHbkiYQn7ucqTGgsO83SkKeA0dy4FuSn2zaVv2DHCZOBVpggod3/xywwRnnMQKMyTl0LFT5eVIKIoZKRpuJkmK8ASNyFDTGHEivXz2SAFPtRLCKBG6YgVn6u+JHHEppzzQneW5ctErxf+8YaaiKy+ncZopEuP5oihjUCWwTAWGVBCs2FQThAXVt0I8RgJhpbNr6BCcxZeXSe/ccmzLubtotm6qOOrgCJyAM+CAS9ACt6ADugCDR/AMXsGb8WS8GO/Gx7y1ZlQzh+APjM8f4VKYkA==</latexit> CP =1.44⇡ <latexit sha1_base64="S8FXUuCZH+7z++hiI9H+ZFAvVqw=">AAACFHicbVDLSgMxFM34rPVVdekmWARBGGakoBuh2I3LCvYBnVIymds2NJkZkoxQhvkIN/6KGxeKuHXhzr8xnc5CWw8EDufcm5wcP+ZMacf5tlZW19Y3Nktb5e2d3b39ysFhW0WJpNCiEY9k1ycKOAuhpZnm0I0lEOFz6PiTxszvPIBULArv9TSGviCjkA0ZJdpIg8q5l9+RSggyLwCuySD1BNFjKXDaaGYZvsauXathL2aDStWxnRx4mbgFqaICzUHlywsimggINeVEqZ7rxLqfEqkZ5ZCVvURBTOiEjKBnaEgEqH6aB8rwqVECPIykOaHGufp7IyVCqanwzeQsr1r0ZuJ/Xi/Rw6t+ysI40RDS+UPDhGMd4VlDOGASqOZTQwiVzGTFdEwkodr0WDYluItfXibtC9t1bPeuVq3fFHWU0DE6QWfIRZeojm5RE7UQRY/oGb2iN+vJerHerY/56IpV7ByhP7A+fwDDMJ3t</latexit> <latexit sha1_base64="S8FXUuCZH+7z++hiI9H+ZFAvVqw=">AAACFHicbVDLSgMxFM34rPVVdekmWARBGGakoBuh2I3LCvYBnVIymds2NJkZkoxQhvkIN/6KGxeKuHXhzr8xnc5CWw8EDufcm5wcP+ZMacf5tlZW19Y3Nktb5e2d3b39ysFhW0WJpNCiEY9k1ycKOAuhpZnm0I0lEOFz6PiTxszvPIBULArv9TSGviCjkA0ZJdpIg8q5l9+RSggyLwCuySD1BNFjKXDaaGYZvsauXathL2aDStWxnRx4mbgFqaICzUHlywsimggINeVEqZ7rxLqfEqkZ5ZCVvURBTOiEjKBnaEgEqH6aB8rwqVECPIykOaHGufp7IyVCqanwzeQsr1r0ZuJ/Xi/Rw6t+ysI40RDS+UPDhGMd4VlDOGASqOZTQwiVzGTFdEwkodr0WDYluItfXibtC9t1bPeuVq3fFHWU0DE6QWfIRZeojm5RE7UQRY/oGb2iN+vJerHerY/56IpV7ByhP7A+fwDDMJ3t</latexit> <latexit sha1_base64="S8FXUuCZH+7z++hiI9H+ZFAvVqw=">AAACFHicbVDLSgMxFM34rPVVdekmWARBGGakoBuh2I3LCvYBnVIymds2NJkZkoxQhvkIN/6KGxeKuHXhzr8xnc5CWw8EDufcm5wcP+ZMacf5tlZW19Y3Nktb5e2d3b39ysFhW0WJpNCiEY9k1ycKOAuhpZnm0I0lEOFz6PiTxszvPIBULArv9TSGviCjkA0ZJdpIg8q5l9+RSggyLwCuySD1BNFjKXDaaGYZvsauXathL2aDStWxnRx4mbgFqaICzUHlywsimggINeVEqZ7rxLqfEqkZ5ZCVvURBTOiEjKBnaEgEqH6aB8rwqVECPIykOaHGufp7IyVCqanwzeQsr1r0ZuJ/Xi/Rw6t+ysI40RDS+UPDhGMd4VlDOGASqOZTQwiVzGTFdEwkodr0WDYluItfXibtC9t1bPeuVq3fFHWU0DE6QWfIRZeojm5RE7UQRY/oGb2iN+vJerHerY/56IpV7ByhP7A+fwDDMJ3t</latexit> <latexit sha1_base64="S8FXUuCZH+7z++hiI9H+ZFAvVqw=">AAACFHicbVDLSgMxFM34rPVVdekmWARBGGakoBuh2I3LCvYBnVIymds2NJkZkoxQhvkIN/6KGxeKuHXhzr8xnc5CWw8EDufcm5wcP+ZMacf5tlZW19Y3Nktb5e2d3b39ysFhW0WJpNCiEY9k1ycKOAuhpZnm0I0lEOFz6PiTxszvPIBULArv9TSGviCjkA0ZJdpIg8q5l9+RSggyLwCuySD1BNFjKXDaaGYZvsauXathL2aDStWxnRx4mbgFqaICzUHlywsimggINeVEqZ7rxLqfEqkZ5ZCVvURBTOiEjKBnaEgEqH6aB8rwqVECPIykOaHGufp7IyVCqanwzeQsr1r0ZuJ/Xi/Rw6t+ysI40RDS+UPDhGMd4VlDOGASqOZTQwiVzGTFdEwkodr0WDYluItfXibtC9t1bPeuVq3fFHWU0DE6QWfIRZeojm5RE7UQRY/oGb2iN+vJerHerY/56IpV7ByhP7A+fwDDMJ3t</latexit> compromise between 1.5pand 0.9p almost no need of compromise eµ =1.35⇡ <latexit 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sha1_base64="j/v4IztRq/zl0bdcVprs4iU7iGE=">AAACCnicbVDLSsNAFJ34rPUVdelmtAiuSuID3QhFNy4r2Ac0IUwmt+3QmSTMTIQSunbjr7hxoYhbv8Cdf+O0zUJbD1w4nHPvzL0nTDlT2nG+rYXFpeWV1dJaeX1jc2vb3tltqiSTFBo04Ylsh0QBZzE0NNMc2qkEIkIOrXBwM/ZbDyAVS+J7PUzBF6QXsy6jRBspsA+8yRu5hGiEvbTPghw8kY3wFXarp+deygK74lSdCfA8cQtSQQXqgf3lRQnNBMSacqJUx3VS7edEakY5jMpepiAldEB60DE0JgKUn0/WGOEjo0S4m0hTscYT9fdEToRSQxGaTkF0X816Y/E/r5Pp7qWfszjNNMR0+lE341gneJwLjpgEqvnQEEIlM7ti2ieSUG3SK5sQ3NmT50nzpOo6VffurFK7LuIooX10iI6Riy5QDd2iOmogih7RM3pFb9aT9WK9Wx/T1gWrmNlDf2B9/gAVf5nT</latexit> <latexit sha1_base64="j/v4IztRq/zl0bdcVprs4iU7iGE=">AAACCnicbVDLSsNAFJ34rPUVdelmtAiuSuID3QhFNy4r2Ac0IUwmt+3QmSTMTIQSunbjr7hxoYhbv8Cdf+O0zUJbD1w4nHPvzL0nTDlT2nG+rYXFpeWV1dJaeX1jc2vb3tltqiSTFBo04Ylsh0QBZzE0NNMc2qkEIkIOrXBwM/ZbDyAVS+J7PUzBF6QXsy6jRBspsA+8yRu5hGiEvbTPghw8kY3wFXarp+deygK74lSdCfA8cQtSQQXqgf3lRQnNBMSacqJUx3VS7edEakY5jMpepiAldEB60DE0JgKUn0/WGOEjo0S4m0hTscYT9fdEToRSQxGaTkF0X816Y/E/r5Pp7qWfszjNNMR0+lE341gneJwLjpgEqvnQEEIlM7ti2ieSUG3SK5sQ3NmT50nzpOo6VffurFK7LuIooX10iI6Riy5QDd2iOmogih7RM3pFb9aT9WK9Wx/T1gWrmNlDf2B9/gAVf5nT</latexit> <latexit sha1_base64="j/v4IztRq/zl0bdcVprs4iU7iGE=">AAACCnicbVDLSsNAFJ34rPUVdelmtAiuSuID3QhFNy4r2Ac0IUwmt+3QmSTMTIQSunbjr7hxoYhbv8Cdf+O0zUJbD1w4nHPvzL0nTDlT2nG+rYXFpeWV1dJaeX1jc2vb3tltqiSTFBo04Ylsh0QBZzE0NNMc2qkEIkIOrXBwM/ZbDyAVS+J7PUzBF6QXsy6jRBspsA+8yRu5hGiEvbTPghw8kY3wFXarp+deygK74lSdCfA8cQtSQQXqgf3lRQnNBMSacqJUx3VS7edEakY5jMpepiAldEB60DE0JgKUn0/WGOEjo0S4m0hTscYT9fdEToRSQxGaTkF0X816Y/E/r5Pp7qWfszjNNMR0+lE341gneJwLjpgEqvnQEEIlM7ti2ieSUG3SK5sQ3NmT50nzpOo6VffurFK7LuIooX10iI6Riy5QDd2iOmogih7RM3pFb9aT9WK9Wx/T1gWrmNlDf2B9/gAVf5nT</latexit> "eµ =0.13 <latexit sha1_base64="6mAeb6NaUQdSho80MgJj+iaa6Ow=">AAACDnicbVDLSsNAFJ34rPUVdelmsBRclUQF3QhFNy4r2Ac0oUwmN+3QyYOZSaGEfIEbf8WNC0Xcunbn3zhNs9DWAxcO59w7c+/xEs6ksqxvY2V1bX1js7JV3d7Z3ds3Dw47Mk4FhTaNeSx6HpHAWQRtxRSHXiKAhB6Hrje+nfndCQjJ4uhBTRNwQzKMWMAoUVoamHWneCMT4OfYmRABiWRcOxk4YZrja2w17POBWbMaVgG8TOyS1FCJ1sD8cvyYpiFEinIiZd+2EuVmRChGOeRVJ5WQEDomQ+hrGpEQpJsVq+S4rhUfB7HQFSlcqL8nMhJKOQ093RkSNZKL3kz8z+unKrhyMxYlqYKIzj8KUo5VjGfZYJ8JoIpPNSFUML0rpiMiCFU6waoOwV48eZl0zhq2juz+ota8KeOooGN0gk6RjS5RE92hFmojih7RM3pFb8aT8WK8Gx/z1hWjnDlCf2B8/gCc3pvD</latexit> <latexit sha1_base64="6mAeb6NaUQdSho80MgJj+iaa6Ow=">AAACDnicbVDLSsNAFJ34rPUVdelmsBRclUQF3QhFNy4r2Ac0oUwmN+3QyYOZSaGEfIEbf8WNC0Xcunbn3zhNs9DWAxcO59w7c+/xEs6ksqxvY2V1bX1js7JV3d7Z3ds3Dw47Mk4FhTaNeSx6HpHAWQRtxRSHXiKAhB6Hrje+nfndCQjJ4uhBTRNwQzKMWMAoUVoamHWneCMT4OfYmRABiWRcOxk4YZrja2w17POBWbMaVgG8TOyS1FCJ1sD8cvyYpiFEinIiZd+2EuVmRChGOeRVJ5WQEDomQ+hrGpEQpJsVq+S4rhUfB7HQFSlcqL8nMhJKOQ093RkSNZKL3kz8z+unKrhyMxYlqYKIzj8KUo5VjGfZYJ8JoIpPNSFUML0rpiMiCFU6waoOwV48eZl0zhq2juz+ota8KeOooGN0gk6RjS5RE92hFmojih7RM3pFb8aT8WK8Gx/z1hWjnDlCf2B8/gCc3pvD</latexit> <latexit sha1_base64="6mAeb6NaUQdSho80MgJj+iaa6Ow=">AAACDnicbVDLSsNAFJ34rPUVdelmsBRclUQF3QhFNy4r2Ac0oUwmN+3QyYOZSaGEfIEbf8WNC0Xcunbn3zhNs9DWAxcO59w7c+/xEs6ksqxvY2V1bX1js7JV3d7Z3ds3Dw47Mk4FhTaNeSx6HpHAWQRtxRSHXiKAhB6Hrje+nfndCQjJ4uhBTRNwQzKMWMAoUVoamHWneCMT4OfYmRABiWRcOxk4YZrja2w17POBWbMaVgG8TOyS1FCJ1sD8cvyYpiFEinIiZd+2EuVmRChGOeRVJ5WQEDomQ+hrGpEQpJsVq+S4rhUfB7HQFSlcqL8nMhJKOQ093RkSNZKL3kz8z+unKrhyMxYlqYKIzj8KUo5VjGfZYJ8JoIpPNSFUML0rpiMiCFU6waoOwV48eZl0zhq2juz+ota8KeOooGN0gk6RjS5RE92hFmojih7RM3pFb8aT8WK8Gx/z1hWjnDlCf2B8/gCc3pvD</latexit> <latexit sha1_base64="6mAeb6NaUQdSho80MgJj+iaa6Ow=">AAACDnicbVDLSsNAFJ34rPUVdelmsBRclUQF3QhFNy4r2Ac0oUwmN+3QyYOZSaGEfIEbf8WNC0Xcunbn3zhNs9DWAxcO59w7c+/xEs6ksqxvY2V1bX1js7JV3d7Z3ds3Dw47Mk4FhTaNeSx6HpHAWQRtxRSHXiKAhB6Hrje+nfndCQjJ4uhBTRNwQzKMWMAoUVoamHWneCMT4OfYmRABiWRcOxk4YZrja2w17POBWbMaVgG8TOyS1FCJ1sD8cvyYpiFEinIiZd+2EuVmRChGOeRVJ5WQEDomQ+hrGpEQpJsVq+S4rhUfB7HQFSlcqL8nMhJKOQ093RkSNZKL3kz8z+unKrhyMxYlqYKIzj8KUo5VjGfZYJ8JoIpPNSFUML0rpiMiCFU6waoOwV48eZl0zhq2juz+ota8KeOooGN0gk6RjS5RE92hFmojih7RM3pFb8aT8WK8Gx/z1hWjnDlCf2B8/gCc3pvD</latexit> ∼ 1.8 sigma preference for NSI 49 Hint of non-zero e e µ from T2K + NO n A 01/10/2025 T2K+NOnA 68%C.L. 90%C.L. Best fit Antonio Palazzo, UNIBA & INFN 49 01/10/2025 T2K and NOnA point to effective couplings of about 0.2. These can be obtained with fundamental couplings on electrons, u and d quarks of a few %. This is still a large number from a theoretical perspective. What theory says about NSI? Neutrinos are components of an SU(2)Ldoublet. Gauge invariance at high energies implies that NSI operators come together with operators involving charged leptons, on which there are strong constraints from CLFV. So, it is very difficult to build models with large NSI Note that forward scattering probes q2= 0 and a light mediator is felt as an heavy one. Hence, also in this case it is legitimate to describe NSI by an effective dim-6 operator. Tree-level see-saw [Forero & Huang 1608.04719] Radiative see-saw [Babu et al. 1907.09498] Light mediators are an appealing alternative Farzan, Heeck 1607.07616 Farzan 1912.09408 Heavy mediators { <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> <latexit sha1_base64="RG03HEwJX1WBjc+2nWlsTV1XmgQ=">AAAB6XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lE0GPRi8cq9gPaUDbbSbt0swm7G6GE/gMvHhTx6j/y5r9x2+agrQ8GHu/NMDMvTAXXxvO+ndLa+sbmVnm7srO7t3/gHh61dJIphk2WiER1QqpRcIlNw43ATqqQxqHAdji+nfntJ1SaJ/LRTFIMYjqUPOKMGis99PK+W/Vq3hxklfgFqUKBRt/96g0SlsUoDRNU667vpSbIqTKcCZxWepnGlLIxHWLXUklj1EE+v3RKzqwyIFGibElD5urviZzGWk/i0HbG1Iz0sjcT//O6mYmug5zLNDMo2WJRlAliEjJ7mwy4QmbExBLKFLe3EjaiijJjw6nYEPzll1dJ66LmezX//rJavyniKMMJnMI5+HAFdbiDBjSBQQTP8Apvzth5cd6dj0VrySlmjuEPnM8fm4SNZQ==</latexit> [Gavela et al. 0809.3451] Some possibilities: Antonio Palazzo, UNIBA & INFN 50