NA61/SHINE experiment for neutrino physics

XXIWorkshoponNeutrinoTelescopes 1stOctober,2025,Padova,Italy NA61/SHINEexperiment forneutrinophysics YusukeKoshio,forNA61/SHINECollaboration (OkayamaUniversity,Japan) 8 TheNA61/SHINEExperiment NA61/SHINE* (SPS*north*area) LHC SPS Over&150&physicists&from&30&institutions&and&15&countries “The SPS Heavy Ion and Neutrino Experiment” <—&CERN&(main&site) Lake&Geneva Geneva&airport Jura&& mountains Y.Nagai 2ndworkshopforatmosphericneutrinoproductionintheMeVtoPeVrange ← NeutrinoTelescopes2025,Padova,Italy Physicsprogram Multi-purposeexperiment •Neutrino:Hadronproductionmeasurements •Stronginteractionphysics •Searchforthecriticalpoint •Studytheonsetofdeconfinement •Studyopen-charmproductionmechanism •Cosmic-rayphysics •Hadronproductionmeasurementstoimproveair-showermodelpredictions •Study(anti-)deuteronproductionmechanismfortheAMSandGAPS •Nuclearfragmentationcrosssectionstounderstandcosmic-rayflux 3 NeutrinoTelescopes2025,Padova,Italy Howtoproduceneutrinobeam 4 B B p π+ µ+ π - p π+π+ µ+ νµ νµ ⇤ <latexit sha1_base64="V5OdF43uFMupWoBdNd3/dbfk9f4=">AAAB7nicdVDLSgMxFL3js9ZX1aWbYBFclZkq6LLoxoWLCvYB7VDuZDJtaCYzJBmhDP0INy4Ucev3uPNvTB9CfR0IHM45l3tzglRwbVz3w1laXlldWy9sFDe3tnd2S3v7TZ1kirIGTUSi2gFqJrhkDcONYO1UMYwDwVrB8Grit+6Z0jyRd2aUMj/GvuQRp2is1Ore2GiIvVLZq7hTEPcX+bLKMEe9V3rvhgnNYiYNFah1x3NT4+eoDKeCjYvdTLMU6RD7rGOpxJhpP5+eOybHVglJlCj7pCFTdXEix1jrURzYZIxmoH96E/Evr5OZ6MLPuUwzwySdLYoyQUxCJn8nIVeMGjGyBKni9lZCB6iQGttQcbGE/0mzWvFOK9Xbs3Ltcl5HAQ7hCE7Ag3OowTXUoQEUhvAAT/DspM6j8+K8zqJLznzmAL7BefsEDnOPYg==</latexit> K+ νe e+ π0 target Primary protons magnetichorn •Primaryinteractionsinthetarget( ) •Secondaryinteractionswithbeamlinematerials(hadrons+C/Be/Al/Ti/Fe/H2Oetc.) •Neutralhadrondecay( ) p+ Be/C →π±, K± p+ Be/C →V0+ X NeutrinoTelescopes2025,Padova,Italy Historyofneutrinoprogram 1. 2006‒2010:p+Cat31GeV/cforT2K 2. 2015‒2018:variousinteractionsat30‒120GeV/cforNuMIandLBNF 3. 2022‒2025:variousinteractionsat30‒120GeV/cforT2K/HK,LBNF/DUNE 5 Twokindsoftargets Thintarget: Afew%ofnuclearinteractionlength tostudysingleinteractions Replicatarget:Samegeometryandmaterial asinrealneutrinobeamline T2K(90cm) NuMI(120cm) NeutrinoTelescopes2025,Padova,Italy NA61/SHINEexperimentalfacility 6 Target •TPCsfortrackinganddE/dx •2dipolemagnetsupto1.5Tfield •Time-of-flightdetectorsplaceddownstream Largeacceptancespectrometerforchargedparticles Momentummeasurement withparticleidentification Analysis of p + T2K replica target data dE/dx [mip] 1 1.5 2 2.5 3 - π - µ - e - Kpd q<0 0.5−00.511.5 1 10 2 10 3 10 q>0 log(p/[GeV/c]) 0.5−0 0.5 1 1.5 + π + µ + e + K p d q>0 Figure 5.13: Energy loss distribution vs. log(p)for the data. The left panel shows the distribution of the negatively charged tracks and the right panel shows the distribution of the positively charged tracks. Energy loss parameterization is overlaid on top of the distributions. relation 5.7 by assuming that a single Gaussian is sufficient for describing the dE/dx distribution in a single phase space bin: f– i(dE/dx;µ–,‡– i)= A– i ‡– iÔ2fiexpA≠(dE/dx≠µ– i)2 2(‡– i)2B.(5.8) clusters n 0 50 100 150 200 250 0 10 20 30 40 50 60 70 80 3 10× (a) clusters n 0 50 100 150 200 250 dE/dx µ/σ 0.00 0.02 0.04 0.06 0.08 0.10 0.12 0.14 (b) Figure 5.14: Distribution of a number of clusters for selected tracks (a) and energy loss resolution with respect to the number of clusters. Resolution saturates around 0.03 for tracks with the large number of clusters. Clusters in the GTPC are not included since energy loss measurement is not performed in the GTPC. Tracks with the low number of clusters may create tails in the dE/dx distribution for a given phase space bin. The possibility of the bias is investigated in subsection 5.5.6. 118 Analysis of p + T2K replica target data dE/dx [mip] 1 1.5 2 2.5 3 - π - µ - e - Kpd q<0 0.5−00.511.5 1 10 2 10 3 10 q>0 log(p/[GeV/c]) 0.5−0 0.5 1 1.5 + π + µ + e + K p d q>0 Figure 5.13: Energy loss distribution vs. log(p)for the data. The left panel shows the distribution of the negatively charged tracks and the right panel shows the distribution of the positively charged tracks. Energy loss parameterization is overlaid on top of the distributions. relation 5.7 by assuming that a single Gaussian is sufficient for describing the dE/dx distribution in a single phase space bin: f– i(dE/dx;µ–,‡– i)= A– i ‡– iÔ2fiexpA≠(dE/dx≠µ– i)2 2(‡– i)2B.(5.8) clusters n 0 50 100 150 200 250 0 10 20 30 40 50 60 70 80 3 10× (a) clusters n 0 50 100 150 200 250 dE/dx µ/σ 0.00 0.02 0.04 0.06 0.08 0.10 0.12 0.14 (b) Figure 5.14: Distribution of a number of clusters for selected tracks (a) and energy loss resolution with respect to the number of clusters. Resolution saturates around 0.03 for tracks with the large number of clusters. Clusters in the GTPC are not included since energy loss measurement is not performed in the GTPC. Tracks with the low number of clusters may create tails in the dE/dx distribution for a given phase space bin. The possibility of the bias is investigated in subsection 5.5.6. 118 M.Pavin,doctoralthesis(2017) topview ResultsinNA61/SHINE NeutrinoTelescopes2025,Padova,Italy Phase1(2006‒2010) ForT2K 8 p p Z2 Z2 Z2 15#θ-bins#for#0#<#θ#<#380#mrad#(Z1-Z5)# 10#θ-bins#for#0#<#θ#<#300#mrad#(Z6) ( ) 4#θ-bins#for#0#<#θ#<#280#mrad#(Z1-Z5)# 2#θ-bins#for#0#<#θ#<#120#mrad#(Z6) ( ) 10#θ-bins#for#0#<#θ#<#380#mrad#(Z1-Z5)# 8#θ-bins#for#0#<#θ#<#260#mrad#(Z6) ( ) NA61/SHINE,Eur.Phys.J.C79,no2100(2019) p + T2K replica at 31 GeV/c data NeutrinoTelescopes2025,Padova,Italy T2Kneutrinofluxuncertainty withNA61/SHINEdata(Phase1) 9 (GeV) ν E 1− 10 1 10 Fractional Error 0 0.1 0.2 0.3 µ νSK: Neutrino Mode, Hadron Interactions Proton Beam Profile & Off-axis Angle Horn Current & Field Horn & Target Alignment Material Modeling Number of Protons Replica 2010 Error Replica 2009 Error Thin Error , Arb. Norm. ν E×Φ µ νSK: Neutrino Mode, T2K Work in Progress Replica! 2009 Replica 2010 T2K,Eur.Phys.J.C83no9782(2023) Improveduncertaintydownto<5% NeutrinoTelescopes2025,Padova,Italy Phase3(2022‒2025) Ongoingandplanned •T2Kreplicatargetrunat31GeV/c(2022) •18timesmoredatathanthepreviousT2Kdataset •Forwardchargedkaons(primaryuncertaintyathigh-energyregion) •K0sproduction(primaryuncertaintyofwrong-signνe) •Fermilabneutrinodata(2023‒2025) •Kaonsonthingraphitetargetsandprotonsonthintitanium(2023) •120GeV/cprotonsonLBNF/DUNEreplicatarget(2024,2025) 16 Futureprospects NeutrinoTelescopes2025,Padova,Italy Low-Energy(<20GeV/c)beamlineproject Possiblephysicstargets 18 •Acceleratorneutrinoexperiments •studysecondaryhadronscatteringsnotcoveredbycurrentdata •Atmosphericneutrinoexperiments •studycosmic-rayprotonscatterings •Spallationneutronsourceneutrinoexperiments •measurementofhadronproductiononp+Hg •Muonexperiments •measurementofhadronproductiononp+Xat8GeV(X=C,W,orheavymaterials) NeutrinoTelescopes2025,Padova,Italy ProspectfortheDUNEexperiment 18 We need to understand the broader energy range of neutrino flux compared to T2K.! -> Phase 2, 3, and future data will help for the reduction of the flux uncertainty! -> Aiming at unprecedented precision, below 2~3% uncertainty on flux prediction DUNE: Eur. Phys. J. C 80, 978 (2020) Laura Fields (NA61++/SHINE Workshop, 2022) Low-Energy(<20GeV/c)beamlineproject Improveneutrinofluxuncertainty 19 T2K/HKfluxuncertainty DUNEfluxuncertainty •Measurementsofsecondaryhadroninteractions bothforacceleratorandatmosphericneutrinos •Needtounderstandthebroadenergyrange •Aimingatbelow2~3%atlast SPSC-M-793:https://cds.cern.ch/record/2810696 Postfit Flux 𝜈𝜈-Mode •HK predicted flux uncertainty prefit (solid) and post IWCD fit (dashed) •Top: right-sign •Bottom: wrong-sign •Improvements to the prior uncertainty do improve the postfit significantly •Particularly notable in wrong-sign 10 Charlie Naseby Imperial College London 8 Aug 2025 Postfit Flux 𝜈𝜈-Mode •HK predicted flux uncertainty prefit (solid) and post IWCD fit (dashed) •Top: right-sign •Bottom: wrong-sign •Improvements to the prior uncertainty do improve the postfit significantly •Particularly notable in wrong-sign 10 Charlie Naseby Imperial College London 8 Aug 2025 Workinprogress Hyper-K(neutrino-focusingmode) νμ¯νμ Currentuncertainty WithLow-Edata NeutrinoTelescopes2025,Padova,Italy Summary •NA61/SHINEhasprovidedcriticaldatatoimproveneutrinoflux predictionsbyprecisehadronproductionmeasurements •Additionaldatataking,includinglowenergyhadroninteractions,are ongoingforfurtherimprovement •Low-energybeamlineisnowconsideredandstudied.Itispromising forunderstandingthehadroninteractionsinvariousexperiments.We areaimingatthefirstbeamafterCERNʼsLong-Shutdown3(2028~) 20