Hadronization model. Teppei Katori Queen Mary University of London CETUP neutrino interaction workshop, Rapid City, SD, USA, July 28, 2014

Transcription

1 Hadronization model model tuning 4. Impact of Hadronization model for PINGU Teppei Katori Queen Mary University of London CETUP neutrino interaction workshop, Rapid City, SD, USA, July 28, 2014 Teppei Katori 07/28/14 1

2 model tuning 4. Impact of hadronization model in PINGU Teppei Katori 07/28/14 2

3 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF ν µ CC cross section per nucleon 3

4 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF K2K ν µ CC cross section per nucleon 4

5 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF K2K MiniBooNE ν µ CC cross section per nucleon 5

6 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF MINOS K2K MiniBooNE ν µ CC cross section per nucleon 6

7 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K MINOS K2K MiniBooNE ν µ CC cross section per nucleon 7

8 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K HyperK ν µ CC cross section per nucleon 8

9 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K HyperK NOvA ν µ CC cross section per nucleon 9

10 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K HyperK NOvA PINGU ν µ CC cross section per nucleon 10

11 Formaggio and Zeller, Rev.Mod.Phys.84(2012) Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K HyperK NOvA LBNF PINGU ν µ CC cross section per nucleon 11

12 Alvarez-Ruso,Hayato,Nieves,ArXiv: Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF 2-10 GeV seems more important, it s the time to understand pion physics! 1. ANL-BNL puzzle 2. CC1π kinematics puzzle 3. Coherent pion production puzzle (4. MiniBooNE CCQE puzzle) (5. MiniBooNE low energy excess) (6. MINERvA target ratio) etc Pion physics hosts 3 open questions of neutrino cross-sections 12

13 1. Next generation neutrino oscillation experiments Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF 2-10 GeV seems more important, it s the time to understand pion physics! - Resonance production - Coherent production - Resonance to DIS transition (shallow inelastic scattering, SIS) - FSI (pion absorption, charge exchange, scattering) - DIS (GRV98, Bodek-Yang correction) - Hadronization 13

14 Grant, Neutrino PINGU (Precision IceCube Next Generation Upgrade) More string in smaller region, but still ~3 Mton - Muon neutrino disappearance measurement for neutrino mass hierarchy (NMH) - Important energy region is 2-10 GeV 14

15 Grant, Neutrino PINGU (Precision IceCube Next Generation Upgrade) More string in smaller region, but still ~3 Mton - Muon neutrino disappearance measurement for neutrino mass hierarchy (NMH) - Important energy region is 2-10 GeV 15

16 Grant, Neutrino PINGU (Precision IceCube Next Generation Upgrade) More string in smaller region, but still ~3 Mton - Muon neutrino disappearance measurement for neutrino mass hierarchy (NMH) - Important energy region is 2-10 GeV 16

17 Akhmedov, Dighe, Lipari, and Smirnov, Nucl.Phys.B542(1999)3 Akhmedov, Razzaque, and Smirnov, JHEP02(2013) PINGU effective 2-ν matter oscillation interference of propagation states Effective 2 neutrino oscillation - P(ν µ à ν µ ) of NMH is equivalent with P(anti-ν µ à anti-ν µ ) of IMH. Propagation state ν e ν e ν µ s 23 ν 3 P A ν 3 s 23 ν µ c 23 ν 2 ν 2 c 23 Cherenkov detector has no charge separation ability. à Is there any information we can use to separate ν µ and anti-ν µ? (or negative muon and positive muon, equivalently) 17

18 Honda, ISVHECRI12 1. Flux Honda flux prediction at the South Pole - ν µ and anti-ν µ show clear difference in angular dependence (vertical muon has shorter propagation length) - The difference becomes larger at high E Zenith angle dependence of atmospheric neutrino flux at the South Pole 18

19 Ribordy and Smirnov, PRD87(2013) Neutrino interaction Inelasticity - It relies on measured hadron energy. - Differential cross section is function of y. - y-dependence of ν µ and anti-ν µ are different. E ν = E µ + E h m N, y = E ν E µ E ν Small y - Better angular resolution Large y - Better ν and anti-ν separation Asymmetry parameter S NI ~ N IH N NH N NH 19

20 Ribordy and Smirnov, PRD87(2013) Neutrino interaction Inelasticity - It relies on measured hadron energy. - Differential cross section is function of y. - y-dependence of ν µ and anti-ν µ are different. E ν = E µ + E h m N, y = E ν E µ E ν Ribordy and Smirnov paper - only DIS is considered. - isonucleon target (n+p) Small y - Better angular resolution Large y - Better ν and anti-ν separation Asymmetry parameter S NI ~ N IH N NH N NH 20

21 Ribordy and Smirnov, PRD87(2013) Neutrino interaction Inelasticity - It relies on measured hadron energy. - Differential cross section is function of y. - y-dependence of ν µ and anti-ν µ are different. E ν = E µ + E h m N, y = E ν E µ E ν Ribordy and Smirnov paper - only DIS is considered. - isonucleon target (n+p) Precise measurement of hadron energy is important. - Quasielastic - Resonance - SIS - Nuclear final state interaction - DIS - Hadronization model 21

22 T2K collaboration, PRD88(2013) Wilking, EPS T2K Multi-pion production = CC other - There are some effort to improve this channel in T2K. - Conservative 30% ~error is assigned. - Significant background for single pion measurement. 22

23 model tuning 4. Impact of hadronization model in PINGU Teppei Katori 07/28/14 23

24 Hadronization in GENIE - Low energy à AGKY model - High energy à PYTHIA6 24

25 AGKY model, EPJC63(2009)1-10 Gallagher, GENIE workshop 2013 Low W hadronization process (AGKY model) - KNO scaling based model - 2.3<W(GeV)<3.0 is used as a window of transition to PYTHIA6. 25

26 AGKY model, EPJC63(2009)1-10 Gallagher, GENIE workshop 2013 Low W hadronization process (AGKY model) - KNO scaling based model - 2.3<W(GeV)<3.0 is used as a window of transition to PYTHIA6. - Agreement with bubble chamber data is good..., better than PYTHIA6 PYTHIA6 only PYTHIA6 only Average charged hadron multiplicity with function of W 2 26

27 Kuzmin and Naumov, PRC88(2013) Low W hadronization process (AGKY model) - KNO scaling based model - 2.3<W(GeV)<3.0 is used as a window of transition to PYTHIA6. - Agreement with bubble chamber data is good..., better than PYTHIA6 - It is a general tendency PYTHIA6 underestimates charged hadron multiplicity NuWro GENIE GiBUU Average charged hadron multiplicity with function of W 2 27

28 Sjostrand, Lonnblad, and Mrenna, hep-ph/ High W hadronization process (PYTHIA6) - Based on JETSET/Lund string model - Used by many experiments (all collider experiments) - Recently, everyone moves to PYTHIA8 A Sketch of fragmentation from q-qbar string breaking 28

29 model tuning 4. Impact of hadronization model in PINGU Teppei Katori 07/28/14 29

30 Rubin, PhD thesis (UIUC) 3. HERMES During NuInt14, Prof. Ulrich Mosel (Giessen) introduced HERMES effort on PYTHIA, and relevant references. - Apparently, HERMES has a long history to tune PYTHIA by their own data - The reason is mentioned in Josh Rubin s thesis Prof. Mosel 30

31 Rubin, PhD thesis (UIUC) 3. HERMES During NuInt14, Prof. Ulrich Mosel (Giessen) introduced HERMES effort on PYTHIA, and relevant references. - Apparently, HERMES has a long history to tune PYTHIA by their own data - The reason is mentioned in Josh Rubin s thesis 31

32 Rubin, PhD thesis (UIUC) 3. HERMES During NuInt14, Prof. Ulrich Mosel (Giessen) introduced HERMES effort on PYTHIA, and relevant references. - Apparently, HERMES has a long history to tune PYTHIA by their own data - The reason is mentioned in Josh Rubin s thesis Lund-scan - Very sophisticated technique is developed Tuned parameters and their correlations 32

33 Rubin, PhD thesis (UIUC) 3. HERMES During NuInt14, Prof. Ulrich Mosel (Giessen) introduced HERMES effort on PYTHIA, and relevant references. - Apparently, HERMES has a long history to tune PYTHIA by their own data - The reason is mentioned in Josh Rubin s thesis Lund-scan - Very sophisticated technique is developed - HERMES data set can be used to tune PYTHIA in GENIE, but we can simply try to use HERMES tuned PYTHIA in GENIE. GENIE hadronization validation tool - Lund-scan parameters are implemented in GENIE-PYTHIA6. - GENIE hadronization validation tool is used to compare with bubble chamber hadron production data 33

34 3. HERMES tuned PYTHIA6 (Lund-scan) Averaged charged hadron multiplicity <n ch > - Lund-scan increases <n ch > (à better agreement with bubble chamber data) both neutrino and antineutrino. Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan 34

35 3. HERMES tuned PYTHIA6 (Lund-scan) Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan Averaged charged hadron multiplicity <n ch > - Lund-scan increases <n ch > (à better agreement with bubble chamber data) both neutrino and antineutrino. neutrino forward and backward charged hadron multiplicity 35

36 3. HERMES tuned PYTHIA6 (Lund-scan) Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan Charged hadron x F distribution - HERMES parameters also improve x F distribution - Seems to me agreement with all charged hadron data are improved neutrino x F anti-neutrino x F with Q2 bin anti-neutrino x F 36

37 3. HERMES tuned PYTHIA6 (Lund-scan) Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan Dispersion of charged hadron multiplicity - Dispersion is unchanged (dispersion is obtained directly from KNO scaling) anti-neutrino neutrino 37

38 3. HERMES tuned PYTHIA6 (Lund-scan) π o multiplicity - HERMES parameters overestimate π o multiplicity - Dispersion is unchanged Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan neutrino anti-neutrino 38

39 3. HERMES tuned PYTHIA6 (Lund-scan) Fragmentation function - HERMES parameters slightly underestimate neutrino high z positive hadrons, negative hadrons are fine - anti-neutrino fragmentation function looks fine (data is sparse) Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan anti-neutrino neutrino neutrino 39

40 3. HERMES tuned PYTHIA6 (Lund-scan) Topological cross section - Transition of AGKY model to PYTHIA6 is visible Red: GENIE v2.8.0 Blue: NuWro Green: Lund-scan anti-neutrino-proton neutrino neutrino-proton neutrino-neutron 40

41 Nowak, NuInt14 3. NuWro Topological cross section - Transition of AGKY model to PYTHIA6 is visible - NuWro does not have this feature (?) neutrino-proton neutrino-neutron 41

42 3. HERMES tuned PYTHIA6 (Lund-scan) On-going work, improve data-genie agreement - average neutral hadron multiplicity - topological cross-sections (- fragmentation function) 42

43 model tuning 4. Impact of hadronization model in PINGU Teppei Katori 07/28/14 43

44 4. Atmospheric neutrino rate prediction GENIE v2.8.0 (1) and (2) à nuclear effect systematics 1. GENIE v2.8.0 with water target (default) (1) and (3) à hadronization systematic error 2. GENIE v2.8.0 with isonucleon target 3. GENIE v2.8.0 with HERMES best fit PYTHIA6 parameters 44

45 4. Atmospheric neutrino rate prediction GENIE v2.8.0 (1) and (2) à nuclear effect systematics 1. GENIE v2.8.0 with water target (default) (1) and (3) à hadronization systematic error 2. GENIE v2.8.0 with isonucleon target 3. GENIE v2.8.0 with HERMES best fit PYTHIA6 parameters Flux weighted cross section for PINGU - flux = 3 different zenith angles (UZ=-1.0, -0.5, 0.0) of Honda flux - Neutrino energy = 2-20 GeV South Pole, Solar Max, -1.0<cosθ<-0.9, 0 o <φ<30 o Preliminary 45

46 4. Atmospheric neutrino rate prediction GENIE v2.8.0 (1) and (2) à nuclear effect systematics 1. GENIE v2.8.0 with water target (default) (1) and (3) à hadronization systematic error 2. GENIE v2.8.0 with isonucleon target 3. GENIE v2.8.0 with HERMES best fit PYTHIA6 parameters Flux weighted cross section for PINGU - flux = 3 different zenith angles (UZ=-1.0, -0.5, 0.0) of Honda flux - Neutrino energy = 2-20 GeV South Pole, Solar Max, -1.0<cosθ<-0.9, 0 o <φ<30 o Blue: Honda flux Red: Extrapolated Honda flux Preliminary 46

47 4. Atmospheric neutrino rate prediction GENIE v2.8.0 (1) and (2) à nuclear effect systematics 1. GENIE v2.8.0 with water target (default) (1) and (3) à hadronization systematic error 2. GENIE v2.8.0 with isonucleon target 3. GENIE v2.8.0 with HERMES best fit PYTHIA6 parameters Flux weighted cross section for PINGU - flux = 3 different zenith angles (UZ=-1.0, -0.5, 0.0) of Honda flux - Neutrino energy = 2-20 GeV Kinematics: - Only particles above Cherenkov threshold are registered - Muon energy, E µ : E ν generator - ω - Hadron energy, E had : total energy of charged hadrons - Neutrino energy, E ν : E ν = E µ +E had -m N - Inelasticity, y: y = (E ν - E µ )/E ν This study is based on generator-level - perfect detector, no particle propagation, no detector simulation - hadronization/nuclear effect might show up only after rigorous detector simulation 47

48 4. Angle measurement cosθ ν cosθ recon black: muon only red: muon+hadron muon only At low energy, muon direction starts to deviate from neutrino direction. IF hadron shower direction is measured, it would improve the angle measurement... muon+hadron 48

49 4. Muon energy black: default GENIE red: HERMES parameter Muon energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Hadronization model difference is a negligible effect 49

50 4. Muon energy black: water target red: isonucleon target Muon energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Nuclear effect is small on muon energy measurement 50

51 4. Hadron energy black: default GENIE red: HERMES parameter Hadron energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Hadronization model difference is a negligible effect 51

52 4. Hadron energy black: water target red: isonucleon target Hadron energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Nuclear effect gives small, but visible effect 52

53 4. Hadron energy black: water target red: isonucleon target Hadron energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Nuclear effect gives small, but visible effect - Neutrino Water target has smaller rate because of less target fraction (=neutrons). - Anti-neutrino water target has higher rate because of more target (=protons). 53

54 4. Hadron energy black: water target red: isonucleon target Hadron energy for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Nuclear effect gives small, but visible effect Overall reduction of cross sections (Pauli blocking), and energy peak is shifted to lower due to neutron emission, nuclear rescattering, absorption, etc. 54

55 4. Inelasticity black: default GENIE red: HERMES parameter Inelasticity for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Hadronization model difference is a negligible effect 55

56 4. Inelasticity black: water target red: isonucleon target Inelasticity for neutrinos with uz=0.0 (horizontal) solid: neutrino dashed: anti-neutrino Nuclear effect gives small, but visible effect in low y region. 56

57 4. Inelasticity black: water target red: isonucleon target Inelasticity for different angle uz= -1.0 (up-going) solid: neutrino dashed: anti-neutrino Nuclear effect gives small, but visible effect in low y region. uz= -0.5 (30 o ) uz= 0.0 (horizontal) 57

58 Hadronization model can be improved by tuning PYTHIA6. HERMES parameters can be used as a start point. We need to improve - neutral hadron multiplicity - topological cross sections ( - fragmentation function?) PINGU is interested in to measure hadronic energy deposit. - Effect of different hadronization model seems small in PINGU physics. - Nuclear target give small, but visible effect in hadron measurement. - Details need to be studied with detector simulation Thank you for your attention! 58

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