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DPF Meeting 2017 July 31 – August 4 Dpf2017.Fnal.Gov Fermilab 1 0 1 Measurement of Neutrino Induced Neutral Current Coherent ⇡

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DPF Meeting 2017 July 31 – August 4 Dpf2017.Fnal.Gov Fermilab 1 0 1 Measurement of Neutrino Induced Neutral Current Coherent ⇡ Neutral Current Coherent π0 Measurement in the NOvA ND Hongyue Duyang University of South Carolina For the NOvA Collaboration DPF Meeting 2017 July 31 – August 4 dpf2017.fnal.gov Fermilab 1 0 1 Measurement of Neutrino Induced Neutral Current Coherent ⇡ 2 Production in the NOvA Near Detector 3 NOvA Authors 4 July 20, 2017 Introduction to Coherent Pion Production 5 Abstract• Neutrinos can coherently scatter off target nucleus via charge/neutral current20 6 We use the NOvA near detector neutrino data corresponding to 3.72 10 proton-on- 0interaction and produce⇥ pions: 7 target to study the neutral current coherent ⇡ production. Neutrino events with only one 0 0 8 visible ⇡ in the final state can result from coherent process, ⌫ ⌫ ⇡ , The signature of 0 0 A ! A 9 coherent ⇡ production is an emergent ⇡ almost• The collinear target withnucleus the incidentstays in neutrino, ground withstate. 10 no other pions or nucleons.This analysis focuses on events with two reconstructed showers 0 • Small momentum transfer. No quantum 11 from the ⇡ decay and no other particles. A data-driven method is developed to provides an number (charge, spin, isospin) exchange. 12 in situ constraint on the background events. The coherent signal is observed as data event 13 excess over non-coherent background MC• in theSingle coherent forward-going region. Clear pion evidence in the final of the 0 14 coherent ⇡ is seen. The Rein-Sehgal model in GENIEstate, no event other generator pions or is usednucleons to determine or 0 15 the selection efficiency. The flux-averaged cross-sectionvertex activity. of the coherent ⇡ is reported. • Coherent π0 is an important background to νe appearance measurement.. 16 1 Introduction • Physics in its own right: Partially Conserved Axial Current (PCAC) 17 Neutrinos can coherently interact with the targethypothesis, nucleus and used produce in Rein-Seghal an outgoing model pion and via in most neutrino event generators such as GENIE. 18 either neutral current (NC) or charge current (CC) interactions. Coherent interaction involves a 19 very small momentum transfer to the target nucleus with no exchange of quantum numbers. The 0 0 20 characteristic of coherent ⇡ production is a single, forward-going ⇡ , with no other final state 0 21 particles or vertex activity. Coherent ⇡ contributes to the background of the ⌫e appearance2 22 oscillation measurement, and the ⌫-e− NC scattering measurement as well. Measurement of 0 0 23 coherent ⇡ production provides a constraint on this ⇡ background. Furthermore, the coherent 24 process has physics interest in its own right. It provides insight into the structure of the weak 25 hadronic current, and the Partially Conserved Axial Current (PCAC) hypothesis [?][?][?]. 0 26 There are relatively few coherent ⇡ measurements. Early bubble chamber results su↵er 27 from low statistics [?][?][?][?][?]. More recently, NOMAD, MiniBooNE, SciBooNE and MINOS Figure 1: Feynman Diagram of the neutrino induced coherent ⇡0 production. (Picture from [?]) 1 The NOvA Near Detector NO�A NO�A Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN) A broad physics scope • 0.3 kton, 4.2mX4.2mX15.8m,Using ��→�e , � ͞ �→� ͞ e … ° Determine the � mass hierarchy • 1 km from source, underground° Determine at theFermilab. �23 octant ° Constrain �CP • PVC cells filled with liquid scintillatorUsing ��→�� ,. � ͞ �→� ͞ � … ° Precision measurements of sin22� and Dm2 . • 23 32 Alternating planes of orthogonal (Exclude view. �23=�/4?) ° Over-constrain the atmos. sector (four oscillation channels) Also … ° Neutrino cross sections at the NO�A Near Detector ° Sterile neutrinos ° Supernova neutrinos Fermilab ° Other exotica Ryan Patterson, Caltech 3 The NOvA Near Detector NOνA Near Detector Construction NO�A NO�A Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN) A broad physics scope • • Detector construction and instrumentation0.3 kton, 4.2mX4.2mX15.8m, completed Aug. Using ��→�e , � ͞ �→� ͞ e … ° Determine the � mass hierarchy 2014 • 1 km from source, underground° Determine at theFermilab. �23 octant ° Constrain �CP • PVC cells filled with liquid scintillatorUsing ��→�� ,. � ͞ �→� ͞ � … • Neutrinos observed within seconds of turning on! ° Precision measurements of sin22� and Dm2 . • 23 32 Alternating planes of orthogonal (Exclude view. �23=�/4?) ° Over-constrain the atmos. sector (four oscillation channels) Also … ° Neutrino cross sections at the NO�A Near Detector ° Sterile neutrinos ° Supernova neutrinos Fermilab ° Other exotica Ryan Patterson, Caltech Beam 11 Jonathan M. Paley 4 The NOvA Near Detector NOνA Near Detector Construction NO�A NO�A Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN) A broad physics scope • • Detector construction and instrumentation0.3 kton, 4.2mX4.2mX15.8m, completed Aug. Using ��→�e , � ͞ �→� ͞ e … ° Determine the � mass hierarchy 2014 • 1 km from source, underground° Determine at theFermilab. �23 octant ° Constrain �CP • PVC cells filled with liquid scintillatorUsing ��→�� ,. � ͞ �→� ͞ � … • Neutrinos observed within seconds of turning on! ° Precision measurements of sin22� and Dm2 . • 23 32 Alternating planes of orthogonal (Exclude view. �23=�/4?) ° Over-constrain the atmos. sector (four oscillation channels) Also … ° Neutrino cross sections at the NO�A Near Detector ° Sterile neutrinos ° Supernova neutrinos Fermilab ° Other exotica 4 cm ⨯ 6 cm Ryan Patterson, Caltech Beam 11 Jonathan M. Paley 5 The NOvA Near Detector NOνA Near Detector Construction NO�A NO�A Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN) A broad physics scope • • Detector construction and instrumentation0.3 kton, 4.2mX4.2mX15.8m, completed Aug. Using ��→�e , � ͞ �→� ͞ e … ° Determine the � mass hierarchy 2014 • 1 km from source, underground° Determine at theFermilab. �23 octant ° Constrain �CP • PVC cells filled with liquid scintillatorUsing ��→�� ,. � ͞ �→� ͞ � … • Neutrinos observed within seconds of turning on! ° Precision measurements of sin22� and Dm2 . • 23 32 Alternating planes of orthogonal (Exclude view. �23=�/4?) ° Over-constrain the atmos. sector Results (four oscillation channels) Also … ° Neutrino cross sections at the NO�A Near Detector Bin to bin correlation matrix: ° Sterile neutrinos ° Supernova neutrinos Fermilab ° Other exotica 4 cm ⨯ 6 cm Ryan Patterson, Caltech Beam Mass weight of detector component: C12 Cl35 H1 Near DetectorTi48 O16 Others 0.3 kton 11 Jonathan M. Paley 66.8% 16.4% 10.5% 206 3.3%layers 2.6% 0.4% 6 The measured inclusive cross section from Gargamelle, T2k, and NOvA as shown. There is also shown the predicted cross section for nue on carbon from GENIE. There is large correlation between the energy bins for NOvA results (see Top table). Our detector material is dominant by the carbon, chlorine, and hydrogen. 11/17 NuInt 2015 Xuebing Bu (Fermilab) 28 The NOvA Near Detector NOνA Near Detector Construction NO�A NO�A Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN) A broad physics scope • • Detector construction and instrumentation0.3 kton, 4.2mX4.2mX15.8m, completed Aug. Using ��→�e , � ͞ �→� ͞ e … ° Determine the � mass hierarchy 2014 • 1 km from source, underground° Determine at theFermilab. �23 octant ° Constrain �CP • PVC cells filled with liquid scintillatorUsing ��→�� ,. � ͞ �→� ͞ � … • Neutrinos observed within seconds of turning on! ° Precision measurements of sin22� and Dm2 . • 23 32 Alternating planes of orthogonal (Exclude view. �23=�/4?) ° Over-constrain the atmos. sector Results (four oscillation channels) Also … ° Neutrino cross sections at the NO�A Near Detector Bin to bin correlation matrix: ° Sterile neutrinos ° Supernova neutrinos Fermilab ° Other exotica 4 cm ⨯ 6 cm Ryan Patterson, Caltech • Low-Z, fine-grained (1 plane ~ 0.15X0), highly-active tracking calorimeter • Optimized for EM shower Beam measurement, including the Mass weight of detector component: π0s C12 Cl35 H1 Near DetectorTi48 O16 Others 0.3 kton 11 Jonathan M. Paley 66.8% 16.4% 10.5% 206 3.3%layers 2.6% 0.4% 7 The measured inclusive cross section from Gargamelle, T2k, and NOvA as shown. There is also shown the predicted cross section for nue on carbon from GENIE. There is large correlation between the energy bins for NOvA results (see Top table). Our detector material is dominant by the carbon, chlorine, and hydrogen. 11/17 NuInt 2015 Xuebing Bu (Fermilab) 28 Coherent π0 in The NOvA ND NOvA ND Data π0 => γπ 0γ => γ γ pi0 Beam Top view Side view • Signature of COH π0 in the NOvA ND is one single forward-going π0. • Photons from neutral pion decay make EM showers. • Reconstructing both photons provide additional constraint on background and energy scale. 8 NuMI off-axis beam NO�A detectors are sited 14 mrad off the NuMI NuMI Beam beam axis The Neutrino Flux With the medium-energy NuMIνµ CC inclusive - Summary of Uncertainties tune, yields a narrow 2-GeV spectrum at the NO�A detectors NOvA Simulation 2.5 0.1 0.08 ➔ Detectors2 are installed by being → Reduces NC and � CC on axis e off beam axis backgrounds in the 14 mrad 0.06 1.5➔ Narrow(NO �bandA) beam peaked at 2 GeV oscillation analyses 0.04 while maintaining ➔ Near maximum oscillation 1 high � flux at 2 GeV. ➔ � Reduced NC background 0.02 Statistical Uncertainty ➔ Reco Muon Kinetic Energy (GeV) Electron neutrino flux counts ~1% 0.5 0 of0.5 total 0.6flux. 0.7 0.8 0.9 1 Reco Cosθµ Ryan Patterson, Caltech • Statistical7 uncertainties areFermilab typically JETP, August< 2% 6, 2015 • Narrow band neutrino beam 1~3GeV peak at ~2GeV, Dominated by νμ (94%) • Systematics• Neutrino are flux still uncertainty being assessed, comes butform we hadron expect production for the differential and beam measurement focusing. ~10% highly correlated (normalization) flux uncertainties, and all others systematics • Hadron production uncertainty constraint by external hadron production data 11/17combined NuInt 2015 to be 5-8%. Xuebing Bu (Fermilab) 5 (PPFX). • σ(E) measurement systematics will be similar, although systematics from energy scale uncertainties will be larger on the rising9 and falling edges of the spectrum. 14 Jonathan M. Paley Analysis Strategy • Select NC π0 sample: no muon track, two photon showers, no other particles.
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