New results from the ICARUS experiment

New results from the ICARUS experiment Christian Farnese INFN Padova [email protected] ICARUS collaboration XXI Workshop on Neutrino Telescopes October 1 st 2025 XXXI International Conference on Neutrino Physics and Astrophysics, June 17 2024 ICARUS at the Short-Baseline Neutrino program: first results D. Gibin, Padova University and INFN on behalf of the ICARUS collaboration COLL Track 1: muon candidate L~2m Beam direction 0.9 m Drift direction 2.1 m wire direction Overlapped cosmic tracks BNB nµCC candidate Track 2 Track 3 COLL Track 1 Track 2 NuMI neCC candidate e-shower (~600 MeV) 0.92 m Drift direction 1 m wire direction Neutrino 2024 - Daniele Gibin 1 . Brookhaven National Lab., USA 2. CERN, Switzerland 3. CINVESTAV, Mexico, 4. Colorado State University, USA 5. Fermi National Accelerator Lab., USA 6. INFN Bologna and University, Italy 7. INFN Catania and University, Italy 8. INFN Genova and University, Italy 9. INFN GSSI, L’Aquila, Italy 10. INFN LNGS, Assergi, Italy 11. INFN LNS, Catania, Italy 12. INFN Milano, Milano, Italy 13. INFN Milano Bic. and University, Italy 14. INFN Napoli, Napoli, Italy 15. INFN Padova and University, Italy 16. INFN Pavia and University, Italy 17. SLAC National Accelerator Lab., USA 18. Southern Methodist University, USA 19. Tufts University, USA 20. University of Chicago, USA 21. University of Houston, USA 22. University of Pittsburgh, USA 23. University of Rochester, USA 24. University of Texas (Arlington),USA 25. INFN Pisa and University, Italy 26. Ramanujan Faculty Phys. Res. India 27. Virginia Tech Institute 28. York University, Canada 29. CBPF, Brazil ICARUS Collaboration at SBN - 2025 Spokesperson: C. Rubbia, GSSI 12 INFN groups, 12 US institutions, CERN, 1 Mexican, 1 Canadian, 1 Indian, 1 Brazilian institutions a On Leave of Absence from INFN Pavia ! P. Abratenko19,N. Abrego-Martinez3, F. Akbar23, L. Aliaga Soplin24, M. Artero Pons15, W.F. Badgett5, L.F. Bagby5, B. Baibussinov15, B. Behera4, V. Bellini7, O. Beltramello2, R. Benocci13, J. Berger4, S. Bertolucci6, M. Betancourt5, K. Biery5, M. Bonesini13, T. Boone4, B. Bottino8, J Bremer2, S. Brice5, V. Brio7, C. Brizzolari13, J. Brown5, H.S. Budd23, A. Campani8, A. Campos27, D. Carber4 , M. Carneiro1, I. Caro Terrazas4, H. Carranza24, R. Castillo Fernandez24, S. Centro15, G. Cerati5, M. Chalifour2, A.Chatterjee26, D. Cherdack21, S. Cherubini11, N. Chitirasreemadam25, M. Cicerchia15, T. Coan18, A. Cocco14, M. R. Convery17, L. Cooper-Troendle22, S. Copello16, H. Da Motta29, A. De Roeck2, S. Di Domizio8, D. Di Ferdinando6, L. Di Noto8, M. Diwan1, S. Dolan2, S. Donati25, R. Doubnik5, F. Drielsma17, J. Dyer4, S. Dytman22, C. Fabre2, A. Falcone13, C. Farnese15, A. Fava5, N. Gallice1, C. Gatto14, M. Geynisman5, D. Gibin15, A. Gioiosa25, W. Gu1, M. Guerzoni6, A. Guglielmi15, G. Gurung24, S. Hahn5, H. Hausner5, A. Heggestuen4, B. Howard28, J. Hrivnak2, C. James5, W. Jang24, Y.-J. Jwa17,L. Kashur4,W. Ketchum5, J.S. Kim23, D.H. Koh17, J. Larkin1, G. Laurenti6,Y. Li1, G. Lukhanin5, C. Mariani27, C. Marshall23, S. Martynenko1, N. Mauri6, A. Mazzacane5 , K.S. McFarland23, D.P. Mendez1, A. Menegolli16, G. Meng15, O.G. Miranda3, D. Mladenov2, N. Moggi6, N.Montagna6, A. Montanari6, C. Montanari5,a, M. Mooney4, G. Moreno Granados3, J. Mueller4, M. Murphy27, D. Naples22, T. Nichols5, S. Palestini2, M. Pallavicini8, V. Paolone22, L. Pasqualini6, L. Patrizii6, L. Paudel4, G. Petrillo17, C. Petta7, V. Pia6, F. Pietropaolo2,a, F. Poppi6, M. Pozzato6, A. Prosser5, G. Putnam20, X. Qian1, A. Rappoldi16, G.L. Raselli16, R. Rechenmacher5, S. Repetto8, F. Resnati2, A.M. Ricci25, E. Richards22, A. Rigamonti2, M. Rosemberg19, M. Rossella16, P. Roy27, C. Rubbia9, M. Saad22, S. Saha22, G. Salmoria29 , G. Savage5, A. Scaramelli16, D. Schmitz20, A. Schukraft5, D. Senadheera22, S.H. Seo5, F. Sergiampietri2, G.Sirri6, J.Smedley23, J. Smith1, A. Soha5, L. Stanco15,H.Tanaka17, F. Tapia24, M. Tenti6, K.Terao17 , F. Terranova13, V.Togo6, D.Torretta5, M.Torti13, R. Triozzi15, Y.T. Tsai17, T. Usher17, F.Varanini15, S. Ventura15, M.Vicenzi1, C. Vignoli10, F.A. Wieler29 , P. Wilson5, R.J. Wilson4, J. Wolfs23, T. Wongjirad19,A.Wood21, E. Worcester1, M. Worcester1, H. Yu1, J. Yu24, A. Zani12, J. Zennamo5, J. Zettlemoyer5, S. Zucchelli6, M. Zuckerbrot5 Slide# : 2Neutrino Telescopes 2025 - Christian Farnese The sterile neutrino puzzle Slide# : 3 Øanti-ne appearance: in anti-nµ accelerator LSND experiment; Combined analysis of Neutrino-4, GALLEX, SAGE, BEST data: Dm142 =7.3 eV2 sin2 (2q14) =0.36 at 5.8 s C.L. (arXiv:2302.09958) Neutrino Telescopes 2025 - Christian Farnese lDespite the well-established 3-flavour n mixing, several anomalies collected so far hinting to additional n states driving oscillations at small distance with Dm2new~O(1 eV2): Øne disappearance: SAGE, GALLEX experiments with Mega-Curie radioactive sources, recently confirmed at 4s by BEST exp. the uncertainties at the oscillation curve (deviation is about 2%–3% of the uncertainties at the oscillation curve). 2. In addition, it should be noted that the experimental points should be fitted with such a sinusoidal dependence, which has a maximum at the origin, since the process of oscillations starts from the source. This significantly reduces the set of sinusoids available for fitting. Figure 47 shows the complete curve of the oscillation process starting from the reactor. There is a maximum at zero; from here, the process of oscillations begins. 3. Below we are trying to perform an additional search for systematic effects connected with the correlated background. We would like to remind that correlated background arise from fast neutrons as a result of elastic and inelastic scattering n; n0. In the reaction of elastic scattering on hydrogen, a recoil proton appears which imitates the signal from a positron. The reaction of inelastic scattering of fast neutrons occurs on carbon nuclei. The fast neutron excites the carbon nucleus, which deexcites before the neutron is thermalized and captured. This process produces a correlated event similar to the IBD process. This looks rather dangerous for the search for neutrino oscillations. However, it should be clarified that the background spectrum is subtracted when we form the on-off difference signal to detect neutrino events. Again, one may be concerned that this subtraction may not be complete due to the effect of background fluctuations associated with fluctuations in atmospheric pressure and temperature since measurements with the reactor running and with the switched off states occur at different times. However, it is possible to quantify this incomplete compensation of the effect. In our case, the measurements have been carried out about for about 4 years and the atmospheric pressure variations that is !1.1% were nicely averaged. Since the reactor on and off operations occurred 87 times, the average contribution of cosmic background fluctuations to the measurement results does not exceed !0.1% or approximately, !ð0.3÷0.5Þ% with respect to the neutrino signal, the oscillations of which are !ð10 ÷15Þ%. So, background fluctuations uncorrelated with the reactor power do not create a danger of a false oscillation effect. Therefore, it is necessary to investigate the possible change in any parameters, correlated with the reactor power. For example, the temperature in the laboratory increases when the reactor is operating. If in this case, for example, the gain of the PMT changes; this will lead to a shift in the spectra. Irregularities in the background spectrum will be shifted. When the background is subtracted, a difference with a periodic structure appears. This reasoning raises the following concern about the possibility of a false oscillation effect. This requires a quantitative assessment of the possible size of the effect. The temperature in the laboratory compartment when the reactor was turned on was not observed to be changing within an accuracy of 1°–2°. It should FIG. 46. Comparison of the R ratio versus L/E for the neutrino signal (top) and the R ratio versus L/E for the background (bottom). FIG. 47. Complete curve of the oscillation process starting from the reactor core center. A. P. SEREBROV et al. PHYS. REV. D 104, 032003 (2021) 032003-30 Ønµdisappearance signal observed by IceCube with best fit Dm412 =3.5 eV2 sin2 (2q24) =0.16 (PRL 133, 201804,2024). ØTension between appearance and disappearance experiments, which are characterized by different n energy range and detection technique. Earth [77–79]. The uncertainty in this process stems from our imperfect knowledge of the neutrino-nucleus cross section [69–73] and the Earth’s composition. To account for this, scale parameters in the νand ¯ νcross sections that alter the Earth absorption [80] have been incorporated. Gaussian priors with 10% width are used to encompass the uncertainties in our energy range. Importantly, this parameter is treated independently of the overall normalization, as a distinct impact of nuclear effects is anticipated in light and heavier targets. Results—The frequentist analysis found the best-fit point at sin2ð2θ24Þ¼0.16 and Δm2 41 ¼3.5eV2. Compared to the standard three-neutrino hypothesis, the test statistic is −2Δlog L¼6.96, yielding a pvalue of 3.1% under the assumption of 2 degrees of freedom. This probability, corresponding to a significance of 2.2σ, does not constitute evidence for the existence of an eV-scale sterile neutrino. To avoid reliance on Wilk’s theorem, the pvalue was alternatively derived using the Feldman-Cousins procedure [81]. We fitted 200 pseudoexperiments generated at the null point, resulting in p¼3%. Moreover, a Bayesian analysis has been conducted (further details available in [34]), and its results align with those obtained through the frequentist approach. The data pulls relative to the best fit are normally distributed for starting and throughgoing events. Furthermore, we do not find large deviations in the pulls using different bin sizes. The goodness of fit was extracted by comparing the observed best-fit likelihood with the likelihood distribution of 500 fits to pseudoexperiments generated assuming the best-fit hypothesis, yielding a pvalue of 12%. Figure 3shows the 90%, 95%, and 99% C.L. contours calculated according to Wilks’theorem. The sensitivity of this analysis was derived using 500 pseudoexperiments, each of which was generated assuming no sterile neutrino model with the nuisance parameters at their central values. The 90% C.L. preferred region of this analysis is consistent with previous results from IceCube [18,19,36]. This result is compared with previous measurements of νμdisappearance from other experiments in Fig. 4. The 90% C.L. allowed region from this result indicates an increased tension with the constraints from long-baseline experiments. The fitted values for the nuisance parameters have very similar behavior for the best-fit sterile and null hypotheses. The nuisance parameter with the largest difference between null and best-fit hypotheses is the overall normalization, pulling −0.05σand 0.41σ, respectively. None of the parameters that model the local response of DOMs, bulk ice properties, and neutrino attenuation pull above 2σor hit their boundary. The same behavior is observed for the parameters that model the neutrino flux, except for two parameters that pull ∼2.3σ: one associated with the cosmicray spectrum and one associated with the spectral index that models nonconventional neutrinos below the pivot energy. The significance of rejecting the null hypothesis remains consistent across various modeling scenarios for the nonconventional component. These scenarios include employing a single power law and introducing additional nuisance parameters on the prompt flux and astrophysical ν=¯ ν. FIG. 3. Frequentist analysis. The 90%, 95%, and 99% C.L. contours, assuming Wilks’theorem, are shown as dotted, dashed, and solid blue lines, respectively. The red bands show the region where 68% and 95% of the pseudoexperiment 99% C.L. observations lie; the red line corresponds to the median. Previous measurements from IceCube [18–20,36,37] at 90% C.L. are shown in gray. FIG. 4. Comparison to other experiments. The 90% and 99% C.L. contours (blue lines) of this analysis compared to 90% C.L. contours from MiniBooNE-SciBooNE [82,83], MINOS [84], CDHS, CCFR [7], and SuperK [85]. PHYSICAL REVIEW LETTERS 133, 201804 (2024) 201804-7 Øanti-ne disappearance signal with a clear L/En ~ 1-3 m/MeV modulation detected by Neutrino-4 experiment at Dimitrovgrad SM-3 reactor. 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 FIG. 24: The Lν/Eνdistribution for events with Rγ>10 and 20 <E e<60 MeV, where Lνis the distance travelled by the neutrino in meters and Eνis the neutrino energy in MeV. The data agree well with the expectation from neutrino background andneutrinooscillationsatlow∆m2. 62 20 TABLE XIV. Results of all six Ga source experiments. Experiment R SAGE-Cr [24]0.95 ±0.12 SAGE-Ar [25]0.79 ±0.095 (+0.09 / -0.10) GALLEX-Cr1 [27]0.953 ±0.11 GALLEX-Cr2 [27]0.812 ±0.11 BEST-Inner 0.791 ±0.05 BEST-Outer 0.766 ±0.05 FIG. 12. Ratios of measured and predicted 71Ge production rates in all Ga source experiments. The combined result is shown as a blue band. i=q2 i,others +(0.032 ⇥Ri)2,(23) and the combined result R0is obtained by the sum R0=Pi(wi·Ri), where wi=(0/i)2and 0= 1/pPi(1/2 i). The result is given as R0±0=0.81 ± 0.03. The total uncertainty is 4.0%. If we consider the correlation between systematic uncertainties, the average value of R0,Cr is obtained first, and then combined with the SAGE-Ar experiment afterward. The uncertainty from the cross section evaluation is the only significant contribution to the correlated uncertainty, and hence the combined result of all six gallium anomaly experiments is given as R0=⇣R Cr ⌘2 ·RCr +⇣R Ar ⌘2 ·RAr ±R,(24) where R=1/p(1/2 Cr +1/2 Ar), RCr =PCr i(wi·Ri), wi=(0/i,others)2,0=1/qPCr i(1/2 i,others) and Cr =0+0.032 ·RCr, with the uncertainty of the total Cr measurements is obtained by summing over. The combined result of all six measurements is obtained as R0=0.80 ±0.047. The total uncertainty is 6.1%, which is larger than the uncorrelated estimation. The result is illustrated in Fig. 12 as a blue band. FIG. 13. Exclusion contours of all gallium anomaly experiments: two GALLEX, two SAGE and two BEST results. The blue solid line and the blue dotted line show the 2and 3 confidence level, respectively. The figure also presents the exclusion contours from Prospect [61], DANSS [62], St´er´eo [63], KATRIN [64], the combined analysis of RENO and NEOS data [65], reactor anti-neutrino anomalies (RAA) [22], interpretations of the MicroBooNE result for the oscillation hypothesis with fixed mixing angle (sin22✓) and profiled over the angle [30], and the model-independent 95% upper bound on sin22✓from all solar neutrino experiments [66]. The 2 allowed region of Neutrino-4 [67] is also presented and the grey shading represents the merged exclusion of the very short baseline (VSBL) null results. Fig. 11 presents the combined result from all gallium source experiments; SAGE, GALLEX and BEST, considering the correlated cross section uncertainties. The best-fit result from the combined analysis of all Ga source experiments is sin22✓=0.34+0.14 0.09,m2=1.25+1 0.25 eV2. Fig. 13 compares the combined result from all gallium anomaly experiments to some other sterile neutrino search experiments. The exclusion curves of Prospect [61], DANSS [62], St´er´eo [63], KATRIN [64], the combined analysis of RENO and NEOS data [65]. One can see that the gallium anomaly result is still in a strong tension with these experiments except a tiny region above 8 eV2. The interpretations of the MicroBooNE result for the oscillation hypothesis either fixed or profiled over the mixing angle (sin22✓)[30] are also presented. These results do not either favor or exclude the allowed region for the gallium anomaly experiments. The 95% allowed region from the reactor antineutrino anomalies (RAA) [22] is also illustrated in the figure. One can see that the tension between the Ga anomalies and the RAA still persists. The figure also shows the 2allowed Short Baseline Neutrino (SBN) at FNAL BNB and NuMi beams Neutrino Telescopes 2025 - Christian Farnese Slide# : 4 Minerba Betancourt 9 J. Nowak, Lancaster University •Rates at SBND: •From Booster: 0.22 Hz (ν) and 0.07 Hz cosmic •Rates at ICARUS: •From Booster 0.03 Hz (ν) and 0.11 Hz cosmic •From NuMI: 0.014 Hz (ν) and 0.08 Hz cosmic 8 LAr TPC facility on the Neutrino Beams at Fermilab BNB f(n)/MeV/m2/106 PoT ICARUS LAr-TPC 600m baseline 470t active volume Taking n data SBND LAr-TPC 110 m baseline 112t active volume Taking n data Booster Neutrino Beam (BNB) arxiv:1503.01520 60 off axis from Main Injector (NuMI) ●ICARUS, SBND Liquid Argon TPCs (LAr-TPC) are installed at 600, 110 m from Booster target, searching for sterile-n oscillations both in appearance and disappearance channels. ●In addition: high-statistics n-Ar cross-section measurements and event identification/ reconstruction studies in view of DUNE: ØMillions/year events in SBND <1 GeV from Booster ØHundred thousands events/year in ICARUS > 1 GeV from off-axis NuMI beam allowing also for a rich Beyond the Standard Model search program. SBN Program: sterile neutrino sensitivity, 3 years (6.6 x1020 pot) lCombined analysis of events collected by ICARUS at far site and by SBND at near using the same LAr-TPC event imaging technology greatly reduces the expected systematics: Ø“Initial” BNB beam composition and spectrum provided by SBND detector, ØHigh ne identification capability of LAr-TPCs rejecting NC event background. Unique capability to study neutrino appearance and disappearance simultaneously nµ disappearance ne appearance ne disappearance Neutrino Telescopes 2025 - Christian Farnese Slide# : 5 SBN is able to achieve a world-leading sensitivity Ø5σ coverage of the parameter area relevant to LSND anomaly ØProbing the parameter area relevant to reactor and gallium anomalies. The ICARUS LAr-TPC detector ØAfter a long R&D by INFN/CERN, the successful operation in 2010-’13 of ICARUS T600 LAr-TPC at the G. Sasso underground lab exposed to CNGS beam, demonstrated the full maturity of this detection technique: lFirst proposed by C. Rubbia in 1977, LAr-TPCs are high granularity, uniform self-triggering detectors with 3D imaging and calorimetric capabilities: ideal detector for nphysics! … paving the way for Long-Baseline experiments Slide: 6Neutrino Telescopes 2025 - Christian Farnese ü2 modules, 2 TPCs per module; ü1.5 m cathode-anode drift, ED= 500 V/cm; ü3 readout wire planes per TPC, in total 54000 wires at 0, ± 600, 3 mm pitch; ü360 8” PMTs behind the wires to detect scintillation light with ns accuracy. Total active mass 476 ton Central cathode E-field cage Wires planes PMTs Eur. Phys. J. C (2023) 83:467 lThe Cosmic Ray Tagger system (CRT) encloses the detector: a double layer of scintillator bars (~1000 m2) tagging incoming cosmics with ~95% efficiency. ICARUS T600 cosmic rejection Side CRT Top CRT Detector installed in the pit before the CRT installation cryo plant details lCosmic g’s and and neutrons are suppressed by ~2.85 m thick concrete overburden installed on top of the CRT, Layer 1 Layer 2 Layer 3 factor ~2 reduction Rate of cosmic rays measured during the overburden installation Slide# : 7Neutrino Telescopes 2025 - Christian Farnese ICARUS operation at FNAL: collected event statistics Slide: 8 Collected Protons on target (PoT)BNB (FHC) positive focusing NuMI (FHC) positive focusing NuMI (RHC) negative focusing RUN-1 (Jun-Jul ‘22) 0.42 1020 0.69 1020 - RUN-2 (Dec ‘22-Jul ‘23) 2.13 1020 2.84 1020 - RUN-3 (Mar –July ‘24) 1.36 1020 - 2.82 1020 RUN-4 (Dec ‘24 – July ‘25) 3.63 1020 - - TOTAL 7.54 1020 3.53 1020 2.82 1020 * No NUMI beam during RUN-4 Neutrino Telescopes 2025 - Christian Farnese lLast neutrino RUN-4 started on Dec. 10 2024 extending to July 8 2025: ØExtraordinary performance of Booster Beam: ~ 3.67 1020 pot delivered to SBN ! Ø3.63 1020 pot collected by ICARUS with an extraordinary 98.7 % efficiency ! lICARUS detector continues to operate with remarkable stability/performance of all components since its initial activation in 2020; lProtons on target collected in the different ICARUS Physics runs: ICARUS performance at FNAL Slide: 9Neutrino Telescopes 2025 - Christian Farnese ØThe cryogenic/purification system performed smoothly with a free electron drift time in LAr tELE ≈ 7-8 ms stable during physics runs: => full track detection efficiency in the whole 1.5 m drift, resulting in a superb neutrino event measurement; QE Electron neutrino interaction Stopping upward going hadron, L ~43 cm Electron shower 76 cm Drift direction 0.72 m Wires Vertex COLLECTION View arXiv:2506.20137v1 ICARUS Work in Progress => A very efficient Trigger down 100 MeV ØEvents are triggered requiring at least Mj = 5 fired PMT pairs inside a 6 m longitudinal T600 slice in coincidence with BNB, NuMI beam spills; ØA 2nd independent/complementary trigger based on total light signal on the fired PMTs was deployed since Run3 to further increase efficiency at low EDEP. Data/MC comparison: 10% of Run2 Data Slide: 16 ICARUS*work*in*progress ICARUS*work*in*progress Pandora Neutrino,energy SPINE Neutrino,energy, ICARUS*work*in*progress ICARUS*work*in*progress Neutrino)Energy)[GeV] Neutrino)Energy)[GeV] lAll plots shown here use 10% of Run 2 data. No data fits have been performed. SPINE Total, transverse, momentum , Total)Transverse)Momentum)[GeV/c] Pandora Total,transverse, momentum Total)Transverse)Momentum)[GeV/c] Data/MC comparison: 10% of Run2 Data– cont. Slide: 17 ICARUS*work*in*progress Entries ICARUS*work*in*progress ICARUS*work*in*progress Pandora Pandora Pandora Entries Entries Muon)kinetic)energy)[GeV] ICARUS*work*in*progress Entries Leading)proton)kinetic)energy)[GeV] ICARUS*work*in*progress SPINE) SPINE) SPINE) Entries Entries ICARUS*work*in*progress lGood agreement for all studied variables in Pandora and SPINE analysis. Angle)muon)leading)proton)qµp Sensitivity for the 1µNp BNB disappearance analysis Slide: 18 lThe nµ disappearance search has now completed the procedure for the signal unblinding for the 100% RUN2 event statistics; ØDetailed Data/Data or Data/MC comparisons and oscillation fit of the Data performed; lBefore starting the unblinding procedure, the 30% of Run 2 data was also used for data/MC comparisons of variables not sensitive to oscillation. lThe 90% confidence level Brazil bands for the Pandora based selection analysis and including all the systematics: lThese sensitivity studies show the potential for discovery of oscillation in the case of a large value of the mass splitting and sterile mixing angle. Stay tuned to see the final analysis result! The contour drawn using the Feldman Cousins critical χ2is under finalization; ICARUS Work in Progress lExcellent statistics to measure cross section for quasi-elastic, resonance and deep inelastic scattering, for both electron and muon neutrinos; lAvailable data ~3.53E20 POT for physics analysis now Expected CC events in the available statistics : nµ 195,000 and ne 10,000. lNeutrino energy spectrum from NuMI at ICARUS covers the first oscillation peak and good coverage of the relevant phase space for DUNE experiment. Neutrino Interactions from NuMI off axis at ICARUS NuMI MCNuMI MC 𝝼μ,8 𝝼μfrom NuMI at ICARUS 𝝼e,8 𝝼efrom NuMI at ICARUS Oscillation probability at DUNE Neutrino Telescopes 2025 - Christian Farnese Slide# : 19 CC 0𝞹analysis – results for the selected sample lFirst analysis targets nµCC 1µNp0p , enhanced in quasi elastic and 2p2h interactions: ØSignal definition: one µ with momentum > 226 MeV/c, any proton with momentum between 400 MeV/c and 1 GeV/c, no p± or p0 in the final state; ØMajor background: events with undetected/misidentified pions. To directly characterize this background an event control sample has been selected with charged pion candidates (requiring the presence of a secondary muon-like track); Neutrino Telescopes 2025 - Christian Farnese Slide# : 20 Minerba Betancourt •First analysis targets 1𝞶+Nproton+0𝜇 -1𝞶+Nproton+0𝜇, N>0 enhanced in quasi-elastic and 2p2h interactions •Building up cross-section analysis to conduct model investigations •Angle between the muon candidate and leading proton candidate populates the phase space somewhat broadly and would be expected to encode information about FSI for all events •Events with contained and exiting muons, efficiency for the uncontained: 34% CC 0𝜇 Selected Sample 15 NuMI Offaxis Meeting / 12 16 Jul 2025 19 100% data; x-sec variables; angular variables lCross section measurement recently completed! lSignal box opening: analyzed exposure is 2.5 1020 POT. ØThe angle between µ and leading p candidates populates broadly the phase space and is expected to encode information about Final State Interactions for all events; Cross section measurement: nµCC 1µNp0p dpT variable lDistributions of the total transverse momentum dpT. Slide: 21 Pre-fit Post-fit Signal Control sample Neutrino Telescopes 2025 - Christian Farnese Results: nµCC 1µNp0p lMeasured cross section as a function of dpT and daT. lThe measurement is compared with the default event generator GENIEv3 Ar23 (shared within SBN and DUNE). Slide: 22 lThe ICARUS measurement of CC0p+proton at higher energy on Argon fills a crucial gap. T2K : lower E on Carbon Hydrogen, MINERvA: higher E on Carbon Hydrogen, µBooNE: lower E on Argon. Neutrino Telescopes 2025 - Christian Farnese Paper under preparation with more cross section measurements and interpretations: stay tuned! Dark sector models investigation by ICARUS lA first search for new particle decaying into di-muon has been recently completed: Strategy:)select)stopping) muon-like)events)which)will) have)a)resolvable)mass)peak clear)final)state,) easily)reconstructed Preliminary A typical µµ event lA rich Beyond Standard Model search program ( DM, heavy neutral leptons,…) has been pursued exploiting the off-axis NuMI beam; lModels considered so far involve dark particles coupling to Standard Model particles via Scalar Portal Interactions: ØHiggs portal Scalar: Scalar dark sector particles, interactions by mixing with Higgs boson; ØHeavy QCD axion: Pseudo-scalar particles, interactions by mixing with pseudo-scalar mesons. Slide# : 23 ØEvents with 2 stopping µs are selected to reconstruct the scalar mass peak: signal expected at small angle to beam (qNuMI <50); ØFlux, interaction model and detector systematic uncertainties have been included. ICARUS Data Preliminary A typical µµ event Strategy:)select)stopping) muon-like)events)which)will) have)a)resolvable)mass)peak clear)final)state,) easily)reconstructed Run 9717 Event 7020 GRAY PUTNAM UNIVERSITY OF CHICAGO 6 𝑀𝜇𝜇: 252 MeV scalar mass peak Search for BSM scalar decays in µ+µwith NuMI - results lOpen box result: 8 events observed, compared to 8 MC expectation, mostly from nµCC coherent p production; lNo new physics signal observed, maximum excess being 0.19 s; lOngoing analysis with uncontained muon candidates to increase the sensitivity; Slide# : 24 PHYSICAL REVIEW LETTERS 134, 151801 (2025) Slide# : 25 dark photon mass coupling dark photon mass dark photon mass coupling coupling IBDM search with ICARUS at LNGS (3 months data) ØExperimental signature: recoil efrom primary interaction and associated ee+ pair from secondary vertex. lA search for Inelastic Boosted Dark Matter using 0.13 kt · y data collected by ICARUS at LNGS, was conducted studying the cosmic interactions out of CNGS n spill: lNo events observed: exclusion limits for several Boosted Dark Matter masses, covering previously unexplored parameter regions. This result is a proof of the LArTPC sensitivity indicating an excellent opportunity for large-scale future experiments, such as DUNE, to greatly expand the parameter space. ØIBDM particle inelasticallly scatters with an ein ICARUS, producing a heavier Dark sector state which decays to Dark Matter particle, emitting a Dark Photon ØDark Photon subsequently couples to a Standard Model photon through kinetic mixing which then converts to e+ ePHYS. REV. D 111, 092003 (2025)