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Accelerator-based neutrinos Lecture 1 Kendall Mahn 26/08/2015, INSS K.Mahn, Acc-nu sources 1 Neutrino sources The Sun (fusion) GalacGc and Our atmosphere extra-galacGc sources (e.g SN) RadioacGve Accelerators decays Reactors 26/08/2015, INSS K.Mahn, Acc-nu sources 2 Neutrino sources The Sun (fusion) GalacGc and Our atmosphere extra-galacGc sources (e.g SN) At solar neutrino energies, mean free path through lead is 1 light year Making precision neutrino measurements require enormous detectors and intense sources RadioacGve Accelerator-driven neutrino beams are one such method Accelerators decays Reactors 26/08/2015, INSS K.Mahn, Acc-nu sources 3 Physics of accelerator based ν experiments Neutrino oscillaon • Measurements of neutrino mixing parameters • Nonstandard neutrino mixing Electroweak tests • Lorentz violaon 2 • Measurement of sin θW • Discovery of νµ, ντ Neutrino interacGons • Charged current interacGons • Neutral current interacGons • Deep inelasGc scaering • Structure funcGons Detector R&D 26/08/2015, INSS K.Mahn, Acc-nu sources 4 Physics of accelerator based ν experiments Neutrino oscillaon K2K, MINOS, T2K, NOvA • Measurements of neutrino mixing parameters OPERA (& ICARUS) • Nonstandard neutrino mixing LSND, Karmen, MiniBooNE, MicroBooNE CHORUS, NOMAD Electroweak tests • Lorentz violaon CCFR, CDHS, NuTeV 2 • Measurement of sin θW Gargamelle, DONUT • Discovery of νµ, ντ CHARM Neutrino interacGons • Charged current interacGons ANL, BNL bubble chamber • Neutral current interacGons experiments • Deep inelasGc scaering SciBooNE, MINERvA • Structure funcGons COHERENT, CONNIE Detector R&D Incomplete list of experiments; later lectures will ArgoNeuT cover future and proposed experiments PEANUT Most experiments cover mul;ple physics topics 26/08/2015, INSS K.Mahn, Acc-nu sources 5 Physics of accelerator based ν experiments Neutrino oscillaon K2K, MINOS, T2K, NOvA • Measurements of neutrino mixing parameters OPERA (& ICARUS) • Nonstandard neutrino mixing LSND, Karmen, MiniBooNE, MicroBooNE Focus for this set of talks CHORUS, NOMAD Electroweak tests • Lorentz violaon CCFR, CDHS, NuTeV 2 • Measurement of sin θW Gargamelle, DONUT • Discovery of νµ, ντ CHARM Neutrino interacGons Neutrino cross secGons covered by K. McFarland • Charged current interacGons ANL, BNL bubble chamber • Neutral current interacGons experiments • Deep inelasGc scaering SciBooNE, MINERvA • Structure funcGons COHERENT, CONNIE Detector R&D Neutrino detecGon techniques covered by K. Scholberg ArgoNeuT PEANUT 26/08/2015, INSS K.Mahn, Acc-nu sources 6 Open quesGons about neutrino mixing Open questions in neutrino mixing # νe & #Ue1 Ue2 Ue3 & # ν1 & Flavor eigenstates % ( % ( % ( Mass eigenstates (coupling to the W) νµ = Uµ1 Uµ2 Uµ 3 ν2 (definite mass) % ( % ( % ( $ ντ ' $Uτ1 Uτ 2 Uτ 3 ' $ν3 ' Unitary PMNS mixing matrix Three observed flavors of neutrinos (νe, νµ , ντ) means U is represented by three independent mixing angles (θ , θ , θ ) and a CP-violang phase δ 12 23 13 Measurements by accelerator-based experiments Is θ23 mixing maximal (θ23=46°±3°) Is there CP viola;on (non- PDG2014 PDG2014 zero δ?) 26/08/2015, INSS K.Mahn, Acc-nu sources 7 Open quesGons about neutrino mixing Open questions in neutrino mixing 3 2 Δm 32 > 0 2 2 2 Δmij = mi − m j 2 2 Δm 21 1 2 Neutrino mass squared (m€ i ) Neutrino oscillaon measurements are sensiGve to the interference of the mass eigenstates (Δm2) Two observed mass “splings”, determined from atmospheric/accelerator and solar/reactor neutrino experiments, respecGvely 2 2 -3 2 § Δm (atmospheric) = |Δm 32|~ 2.4 x 10 eV 2 2 -5 2 § Δm (solar) = Δm 21 ~ 7.6 x 10 eV 26/08/2015, INSS K.Mahn, Acc-nu sources 8 Open quesGons about neutrino mixing Open questions in neutrino mixing 3 2 2 Δm 21 2 Δm 32 > 0 1 m2 2 Δ 32 < 0 2 Δm 21 1 3 2 Neutrino mass squared (mi ) 2 The sign of Δm 32, or the “mass hierarchy” is sGll unknown 2 § Normal “hierarchy” is like quarks (m1 is lightest, Δm 32 >0 ) 2 § Inverted hierarchy has m3 lightest (Δm 32 <0) What is the mass hierarchy? 26/08/2015, INSS K.Mahn, Acc-nu sources 9 Oscillaon probabiliGes Oscillation probabilities 2 2 |Δm 32| >> Δm 21, producing high frequency and low frequency oscillaon terms ( 1.27Δm2 L + ( 2.54Δm2 L+ P 4 Re U U * U * U sin2 ij 2 Im U U * U * U sin ij αβ = δαβ − ∑ [ βi αi βj αj ] * - + ∑ [ βi αi βj αj ] * - i> j ) E , i> j ) E , 2 2 2 If choose L, E, such that sin (Δm 32L/E) is of order 1, then Δm 21 terms will be € small. Then... ν “disappear’’ into ν , ν µ e τ ( 1.27 m2 L + 2 2 Δ 32 P(νµ → ν µ ) ≅ 1− sin 2θ23 sin * - ) E , A small amount of νe will “appear’’ 2 2 Δm 31 ~ Δm 32 € 2 2 2 2 ' 1.27Δm31L * P(νµ → νe ) ≅ sin 2θ13 sin θ23 sin ) , ( E + Only leading order terms shown 26/08/2015, INSS K.Mahn, Acc-nu sources 10 € Accelerator-basedAccelerator based neutrino neutrino sources sources 95m Decay region Neutrino beam π+ 30 GeV Carbon 3 MagneGc Pions and kaons Beam Proton beam Target focusing decay to neutrinos dump ``horns” To measure νµ disappearance, and νe appearance requires a νµ source* § Atmospheric neutrinos include both νe and νµ from producon § Accelerator based beams are pure νµ from a proton -> meson -> decay chain: § Typically >99.9% νµ § ProducGon of neutrinos is “known”, scalable with accelerator improvements § Also possible to create anGneutrino source *There are other ways to probe oscilla;on physics with intense sources, more later 26/08/2015, INSS K.Mahn, Acc-nu sources 11 Oscillaon probabiliGes Oscillation probabilities νµ to νe appearance probability expansion: E A =2 √2G N ν F e ∆m2 32 Key players: 2 -3 2 § |Δm 32|~ 2.4 x 10 eV (atmospheric mass spling) § Mixing angles: θ12, θ23, θ13 Approxima;on from § CP-violang phase δCP M. Freund, PRD 64, 053003 Neutrinos vs. anneutrinos probability depends on δCP, mass hierarchy (sign 2 of Δm 32 ) • Mass hierarchy is determined through energy dependence of νe, νµ interacGons in maer (maer effects, A terms) 26/08/2015, INSS K.Mahn, Acc-nu sources 12 Oscillaon probabiliGes Oscillation probabilities νµ to νe appearance probability expansion: E A =2 √2G N ν F e ∆m2 32 Key players: 2 -3 2 § |Δm 32|~ 2.4 x 10 eV (atmospheric mass spling) § Mixing angles: θ12, θ23, θ13 Approxima;on from § CP-violang phase Subleading terms of δCPνµ to νe appearance depend on δCP, mass hierarchy, but interpretaon requires precision measurements of: M. Freund, PRD 64, 053003 Δm2 , θ (disappearance) and Δm2 , θ and θ Neutrinos vs. anneutrinos probability depends on 32 23 21 δ12CP, mass hierarchy13 (sign 2 of Δm 32 ) Measurements of νµ to νe (and νµ to νe ) appearance are sensi;ve to • Mass hierarchy is determined through energy dependence of currently unknown physics νe, νµ interacGons in maer (maer effects, A terms) 26/08/2015, INSS K.Mahn, Acc-nu sources 13 Oscillation probabilities 2 2 2 ( 1.27Δm32 L + P(νµ → ν µ ) ≅ 1− sin 2θ23 sin * - ) E , 2 2 Measure: Δm 32 and sin 2θ23 Experimental controls: § Fix beam energy (E) € § Place a detector at L, the (first) oscillaon maximum Why not place two detectors, one at L and one at 2L? P(ν ) µ Flux decreases as 1/L2: Osc maximum Event rate scales with flux: N = Φ x σ x ε P(ν ) ξ Event rate is (currently) too small 26/08/2015, INSS K.Mahn, Acc-nu sources KARMEN website graphic 14 Long baseline experiments 2 2 2 ( 1.27Δm32 L + P(νµ → ν µ ) ≅ 1− sin 2θ23 sin * - +... ) E , Unknown road to Unknown road - Google Maps http://maps.google.com/maps?hl=en&tab=wl Δm2 ~3x10-3 eV2, want sin2(Δm2 L/E) to be of order 1 32 To see all the details that are visible on the screen, use the "Print" link next to the map. Tokai To € Kamioka (T2K) experiment: MINOS experiment: Eν(peak) ~0. 6GeV, L=295km Eν(peak) ~3 GeV, L=735km First part of lecture: What are the physics results from long baseline experiments? ©2011 Google - Imagery ©2011 TerraMetrics - 26/08/2015, INSS K.Mahn, Acc-nu sources 15 1 of 1 4/23/11 10:27 AM Accelerator-basedThe Tokai-to- Kamiokaexperiment experiment example: T2K The physics so far: νµ to νe (and νµ to νe) appearance: § Discovery of νe appearance (2013) § Search for presence of appearance Neutrino flux at SK with anGneutrinos; necessary step (no oscillaon) toward future CPV searches νµ, νµ disappearance: § World’s best measurement of θ23 § With anGneutrinos: test of NSI or CPT theorem 26/08/2015, INSS K.Mahn, Acc-nu sources 16 νµ disappearance at T2K For a fixed baseline (L=295km) 2 2 2 ( 1.27Δm32 L + oscillaon probabiliGes depend on P(νµ → ν µ ) ≅ 1− sin 2θ23 sin * - +... ) E , the neutrino energy Eν 2 2 Data Extract Δm , sin θ23 from observed 60 change in overall rate and spectrum MC€ Unoscillated Spectrum 40 MC Best Fit Spectrum § Energy esGmated using lepton NC MC Prediction Events/0.10 GeV momentum, angle and assumed 20 CCQE kinematcs 0 0 2 4 > 5 PRD 91, 072010 (2015) Reconstructed ν Energy (GeV) 10 1 10−1 10−2 0 2 4 > 5 Osc. to unosc Events/0.1 GeV Reconstructed ν Energy (GeV) 26/08/2015, INSS K.Mahn, Acc-nu sources 17 T2K observed event distributions) 4 /c 2 T2K data favors maximal disappearance 3.2 eV -3 § Provides best constraint on θ to date, SK joint OA 23 (10 3 consistent with maximal (45°) mixing 2 32 m ∆ 2.8 T2K joint OA 2.6 2.4 2.2 MINOS joint OA 0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7 ) 4 -2 /c 2 eV -3 -2.2 MINOS joint OA (10 2 32 PRD 91, 072010 (2015) m -2.4 ∆ -2.6 -2.8 T2K joint OA -3 SK joint OA 0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7 2 sin θ23 26/08/2015, INSS 18 K.Mahn, Acc-nu sources T2K observed event distributions) 4 /c 2 T2K data favors maximal disappearance 3.2 eV -3 § Provides best constraint on θ to date, SK joint OA 23 (10 3 consistent with maximal (45°) mixing 2 32 m ∆ § Atmospheric measurements also 2.8 T2K joint OA important (SK, IceCube) 2.6 Best constraint on mass spling from MINOS experiment 2.4 • Energy uses lepton and hadronic state 2.2 MINOS joint OA 0.3 0.35 0.4 0.45 0.5 0.55 0.6 0.65 0.7 ) 4 -2 /c 2 eV -3 -2.2 MINOS joint OA (10 2 32 PRD 91, 072010 (2015) m -2.4 ∆ -2.6 -2.8 T2K joint OA -3 SK joint OA Phys.
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  • Determination of the Νµ-Spectrum of the CNGS Neutrino Beam by Studying Muon Events in the OPERA Experiment

    Determination of the Νµ-Spectrum of the CNGS Neutrino Beam by Studying Muon Events in the OPERA Experiment

    Determination of the νµ-spectrum of the CNGS neutrino beam by studying muon events in the OPERA experiment Diplomarbeit der Philosophisch-naturwissenschaftlichen Fakultät der Universität Bern vorgelegt von Claudia Borer 2008 Leiter der Arbeit: Prof. Dr. Urs Moser Laboratorium für Hochenergiephysik Contents Introduction 1 1 Neutrino Physics 3 1.1 History of the Neutrino . 3 1.2 The Standard Model of particles and interactions . 6 1.3 Beyond the Standard Model . 12 1.3.1 Sources for neutrinos . 14 1.3.2 Two avour neutrino oscillation in vacuum . 14 1.3.3 Three avour neutrino oscillation in vacuum . 17 1.3.4 Neutrino oscillation in matter . 20 2 The OPERA experiment 23 2.1 Expected physics performance . 24 2.1.1 Signal detection eciency . 24 2.1.2 Expected background . 25 2.1.3 Sensitivity to νµ → ντ oscillations . 26 2.2 The CNGS neutrino beam . 27 2.3 The OPERA detector . 28 2.3.1 Emulsion target . 29 2.3.2 The Target Tracker . 31 2.3.3 The muon spectrometers . 33 2.3.4 The veto system . 35 2.3.5 Data acquisition system (DAQ) . 37 3 Analysis methods 39 3.1 Kalman ltering . 39 3.2 Monte Carlo samples . 42 3.3 Producing histogramms . 46 3.4 Unfolding method based on Bayes' Theorem . 47 i ii CONTENTS 4 Physical results 51 Conclusion 57 A Two avour neutrino oscillation in vacuum 59 Acknowledgement 61 List of Figures 63 List of Tables 65 Bibliography 67 Introduction The Standard Model (SM) of particles and interactions successfully describes particle physics. In the last years growing evidence has been established, indicating that the SM must be extended to possibly include new physics.