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DUNE: The Deep Underground Neutrino Experiment Mark Thomson University of Cambridge & co-spokesperson of DUNE Birmingham HEP Seminar: 4 th May 2016 Topic Slides 1: Context: The 2012 Revolution 1 2: Why are neutrinos so important 2

  1. Neutrino Oscillations in Matter « Accounting for this potential term, gives a Hamiltonian that is not diagonal in the basis of the mass eigenstates         | ν 1 i | ν 1 i 0 0 | ν 1 i E 1  = i d ME                         | ν 2 i | ν 2 i | ν 2 i H 0 E 2 0  + V | ν e i          =                 d t                 | ν 3 i | ν 3 i | ν 3 i 0 0 E 3      « Complicates the simple picture !!!! What we measure P ( ν µ → ν e ) − P ( ν µ → ν e ) = ∆ m 2   31 L 16 A ME sin 2  c 2 13 s 2 13 s 2 23 (1 − 2 s 2   Small 13 )       ∆ m 2 4 E  31 ∆ m 2   31 L − 2 AL ME  c 2 13 s 2 13 s 2 23 (1 − 2 s 2   Proportional to L sin 13 )       E 4 E  − 8 ∆ m 2 ∆ m 2 What we want   21 L 31 L CPV sin 2  sin δ · s 13 c 2   13 c 23 s 23 c 12 s 12       2 E 4 E  √ E ρ with 2 G F n e E = 7 . 6 × 10 − 5 eV 2 · A = 2 g cm − 3 · GeV 20 04/05/2016 Mark Thomson | DUNE

  2. Experimental Strategy EITHER: « Keep L small (~200 km): so that matter effects are insignificant § First oscillation maximum: ∆ m 2 31 L ∼ π E ν < 1 GeV 4 E 2 § Want high flux at oscillation maximum Off-axis beam: narrow range of neutrino energies OR: « Make L large (>1000 km): measure the matter effects (i.e. MH) § First oscillation maximum: ∆ m 2 31 L ∼ π E ν > 2 GeV 4 E 2 § Unfold CPV from Matter Effects through E dependence On-axis beam: wide range of neutrino energies 21 04/05/2016 Mark Thomson | DUNE

  3. Experimental Strategy EITHER: « Keep L small (~200 km): so that matter effects are insignificant § First oscillation maximum: ∆ m 2 31 L ∼ π E ν < 1 GeV 4 E 2 § Want high flux at oscillation maximum Off-axis beam: narrow range of neutrino energies OR: « Make L large (>1000 km): measure the matter effects (i.e. MH) § First oscillation maximum: ∆ m 2 31 L ∼ π E ν > 2 GeV 4 E 2 § Unfold CPV from Matter Effects through E dependence On-axis beam: wide range of neutrino energies 22 04/05/2016 Mark Thomson | DUNE

  4. 5. DUNE 23 04/05/2016 Mark Thomson | DUNE

  5. DUNE in a Nutshell « Intense beam of or fired 1300 km at a large detector ν µ ν µ « Compare and oscillations ν µ → ν e ν µ → ν e « Probe fundamental differences between matter & antimatter ν µ ν e ν τ ν τ ν µ ν τ ν µ ν µ ν µ 24 04/05/2016 Mark Thomson | DUNE

  6. DUNE in a Larger Nutshell « LBNF/DUNE § Muon neutrinos/anti-antineutrinos from high-power proton beam • 1.2 MW from day one • upgradable to 2.4 MW § Large underground LAr detector at Sanford Underground Research Facility (SURF) in South Dakota • 4 Cavern(s) for ≥ 40 kt total fiducial far detector mass • 10 - 20 kt fiducial LAr Far Detector (from day one) • 40 kt as early as possible § Highly-capable Near Detector system • Using one or more technologies 25 04/05/2016 Mark Thomson | DUNE

  7. LBNF/DUNE – Fermilab in 2025 26 04/05/2016 Mark Thomson | DUNE

  8. LBNF/DUNE – Fermilab in 2025 27 04/05/2016 Mark Thomson | DUNE

  9. Origins of DUNE P5 strategic review of US HEP • Called for the formation of “LBNF”: – as a international collaboration bringing together the international neutrino community – ambitious scientific goals with discovery potential for: • Leptonic CP violation • Proton decay • Supernova burst neutrinos Resulted in the formation of the DUNE collaboration with strong representation from: – LBNE (mostly US) – LBNO (mostly Europe) – Other interested institutes 28 04/05/2016 Mark Thomson | DUNE

  10. DUNE: rapid progress Things are moving very fast… • First formal collaboration meeting April 16 th -18 th 2015 – Over 200 people attended in person • Conceptual Design Report in June (foundations from LBNE/LBNO) • Passed DOE CD-1 Review in July • Second collaboration meeting September 2 nd -5 th 2015 • Successful CD-3a Review in December 2015 – paves the way to approval of excavation in FY17 29 04/05/2016 Mark Thomson | DUNE

  11. DUNE has strong support from: • Fermilab and US DOE: – This is the future flagship project for Fermilab – “no plan B” • CERN – Very significant agreements on CERN – US collaboration + Strong international interest: Brazil, India, Italy, Switzerland, UK, … 30 04/05/2016 Mark Thomson | DUNE

  12. The DUNE Collaboration As of today: from 856 Collaborators 149 Institutes USA USA UK India Italy Other India UK Other Italy Switzerland Brazil Spain France France Americas Brazil Poland Americas Switzerland Poland Spain Czech Republic Czech Republic DUNE has broad international support 31 04/05/2016 Mark Thomson | DUNE

  13. 5.1 DUNE Science Strategy Unprecedented precision utilizing a massive Liquid Argon TPC ν A neutrino interaction in the ArgoNEUTdetector at Fermilab 32 04/05/2016 Mark Thomson | DUNE

  14. DUNE Primary Science Program Focus on fundamental open questions in particle physics and astroparticle physics: • 1) Neutrino Oscillation Physics – Discover CP Violation in the leptonic sector – Mass Hierarchy – Precision Oscillation Physics: • e.g. parameter measurement, θ 23 octant, testing the 3-flavor paradigm • 2) Nucleon Decay p → K + ν – e.g. targeting SUSY-favored modes, • 3) Supernova burst physics & astrophysics – Galactic core collapse supernova, sensitivity to ν e 33 04/05/2016 Mark Thomson | DUNE

  15. DUNE Primary Science Program Focus on fundamental open questions in particle physics and astroparticle physics: • 1) Neutrino Oscillation Physics – Discover CP Violation in the leptonic sector – Mass Hierarchy – Precision Oscillation Physics: • e.g. parameter measurement, θ 23 octant, testing the 3-flavor paradigm • 2) Nucleon Decay p → K + ν – e.g. targeting SUSY-favored modes, • 3) Supernova burst physics & astrophysics – Galactic core collapse supernova, sensitivity to ν e 34 04/05/2016 Mark Thomson | DUNE

  16. Long Baseline (LBL) Oscillations Measure neutrino spectra at 1300 km in a wide-band beam ν µ ν µ µ & ν e STT'Module' Barrel' Backward'ECAL' Barrel'' ECAL' RPCs' FD End' Magnet' RPCs' Coils' Forward' ECAL' End' RPCs' ND • Near Detector at Fermilab: measurements of ν µ unoscillated beam • Far Detector at SURF: measure oscillated ν µ & ν e neutrino spectra 35 04/05/2016 Mark Thomson | DUNE

  17. Long Baseline (LBL) Oscillations … then repeat for antineutrinos • Compare oscillations of neutrinos and antineutrinos • Direct probe of CPV in the neutrino sector ν µ ν µ µ & ν e STT'Module' Barrel' Backward'ECAL' Barrel'' ECAL' RPCs' FD End' Magnet' RPCs' Coils' Forward' ECAL' End' RPCs' ND • Near Detector at Fermilab: measurements of ν µ unoscillated beam • Far Detector at SURF: measure oscillated ν µ & ν e neutrino spectra 36 04/05/2016 Mark Thomson | DUNE

  18. 3.2 Proton Decay Proton decay is expected in most new physics models • But lifetime is very long, experimentally τ > 10 33 years • Watch many protons with the capability to see a single decay • Can do this in a liquid argon TPC – For example, look for kaons from SUSY-inspired GUT p-decay p → K + ν modes such as cathode kaon�decay muon�decay time E ~ O(200 MeV) wire�no. 0.5�m 37 04/05/2016 Mark Thomson | DUNE

  19. Proton Decay Proton decay is expected in most new physics models • But lifetime is very long, experimentally τ > 10 33 years • Watch many protons with the capability to see a single decay • Can do this in a liquid argon TPC – For example, look for kaons from SUSY-inspired GUT p-decay p → K + ν modes such as Remove incoming particle cathode § Clean signature very low backgrounds kaon�decay muon�decay “simulated” time p-decay 1 Mt.yr wire�no. 0.5�m 38 04/05/2016 Mark Thomson | DUNE

  20. Supernova ν s A core collapse supernova produces an incredibly intense burst of neutrinos • Measure energies and times of neutrinos from galactic supernova bursts – In argon (uniquely)the largest sensitivity is to ν e ν e + 40 Ar → e − + 40 K ∗ Energy time Events per bin Events per 0.5 MeV Infall Neutronization Accretion Cooling 40 ES ES 40 70 40 Ar Ar ν ν 35 e e 40 40 ν Ar ν Ar e 60 e 30 E ~ O(10 MeV) 50 25 20 40 15 30 10 20 5 10 0 5 10 15 20 25 30 35 40 Observed energy (MeV) 0 -2 -1 Physics Highlights include: 10 10 1 Time (seconds) § Possibility to “see” neutron star formation stage Even the potential to see black hole formation ! § 39 04/05/2016 Mark Thomson | DUNE

  21. 6: DUNE Neutrino Physics 40 04/05/2016 Mark Thomson | DUNE

  22. DUNE Oscillation Strategy Measure neutrino spectra at 1300 km in a wide-band beam • Determine MH and θ 23 octant, probe CPV, test 3-flavor paradigm a and search for BSM effects (e.g. NSI) in a single experiment – Long baseline: • Matter effects are large ~ 40% E ~ few GeV – Wide-band beam: • Measure ν e appearance and ν µ disappearance over range of energies • MH & CPV effects are separable ν µ / ν µ disappearance ν e / ν e appearance 800 350 120 35 DUNE ν disappearance DUNE ν disappearance DUNE ν appearance DUNE ν appearance µ µ e e 150 kt-MW-yr ν mode 150 kt-MW-yr ν mode 150 kt-MW-yr ν mode 150 kt-MW-yr ν mode 2 2 700 sin ( θ )=0.45 Signal ν CC sin ( θ )=0.45 Signal ν CC Normal MH, δ =0 Normal MH, δ =0 300 30 µ 23 23 µ CP CP 100 2 2 Bkgd ν CC sin ( )=0.45 sin ( )=0.45 NC θ θ µ 23 23 ( + ) CC ν ν NC τ τ 600 Signal ( ν + ν ) CC Signal ( ν + ν ) CC Bkgd ν CC ( + ) CC e e e e ν ν Events/0.25 GeV µ Events/0.25 GeV 250 τ τ Events/0.25 GeV Events/0.25 GeV 25 Beam ( ν + ν ) CC Beam ( ν + ν ) CC CDR Reference Design CDR Reference Design e e e e 80 NC NC Optimized Design Optimized Design 500 ( ν + ν ) CC ( ν + ν ) CC τ τ τ τ 200 ( ν + ν ) CC 20 ( ν + ν ) CC µ µ µ µ CDR Reference Design CDR Reference Design 400 60 Optimized Design Optimized Design 150 15 300 40 100 10 200 20 50 5 100 0 0 0 0 1 2 3 4 5 6 7 8 1 2 3 4 5 6 7 8 1 2 3 4 5 6 7 8 1 2 3 4 5 6 7 8 Reconstructed Energy (GeV) Reconstructed Energy (GeV) Reconstructed Energy (GeV) Reconstructed Energy (GeV) 41 04/05/2016 Mark Thomson | DUNE

  23. MH Sensitivity « Sensitivities depend on multiple factors: § Other parameters, e.g. δ § Beam spectrum, … 40 CDR Reference Design MH 35 Optimized Design MH significance 30 0% 25 2 χ 50% 20 ∆ 15 100% 10 5 0 0 200 400 600 800 1000 1200 1400 Exposure (kt-MW-years) 42 04/05/2016 Mark Thomson | DUNE

  24. MH Sensitivity « Sensitivities depend on multiple factors: § Other parameters, e.g. δ § Beam spectrum, … 40 CDR Reference Design MH 35 Optimized Design MH significance 30 0% 25 2 χ 50% 20 ∆ 15 100% 10 5 0 0 200 400 600 800 1000 1200 1400 Exposure (kt-MW-years) 43 04/05/2016 Mark Thomson | DUNE

  25. MH and CPV Sensitivities « Sensitivities depend on multiple factors: § Other parameters, e.g. δ § Beam spectrum, … 40 12 CDR Reference Design CPV MH CDR Reference Design 35 Optimized Design Optimized Design 10 CPV significance MH significance 30 25% 0% 8 25 50% 2 χ 2 χ 50% ∆ 20 ∆ 6 = σ 15 4 75% 100% 10 2 5 0 0 0 200 400 600 800 1000 1200 1400 0 200 400 600 800 1000 1200 1400 Exposure (kt-MW-years) Exposure (kt-MW-years) 44 04/05/2016 Mark Thomson | DUNE

  26. MH and CPV Sensitivities « Sensitivities depend on multiple factors: § Other parameters, e.g. δ § Beam spectrum, … 40 12 CDR Reference Design CPV MH CDR Reference Design 35 Optimized Design Optimized Design 10 CPV significance MH significance 30 25% 0% 8 25 50% 2 χ 2 χ 50% ∆ 20 ∆ 6 = σ 15 4 75% 100% 10 2 5 0 0 0 200 400 600 800 1000 1200 1400 0 200 400 600 800 1000 1200 1400 Exposure (kt-MW-years) Exposure (kt-MW-years) 45 04/05/2016 Mark Thomson | DUNE

  27. Beyond discovery: measurement of δ « CPV “coverage” is just one way of looking at sensitivity… « Can also express in terms of the uncertainty on δ Start to ~approach current level of precision on quark-sector CPV phase (although takes time) 46 04/05/2016 Mark Thomson | DUNE

  28. Timescales: year zero = 2025 Rapidly reach scientifically interesting sensitivities: – e.g. in best-case scenario for Mass Hierarchy : • Reach 5 σ MH sensitivity with 20 – 30 kt.MW.year ~2 years Discovery – e.g. in best-case scenario for CPV ( δ CP = + π /2) : • Reach 3 σ CPV sensitivity with 60 – 70 kt.MW.year Strong evidence ~3-4 years – e.g. in best-case scenario for CPV ( δ CP = + π /2) : • Reach 5 σ CPV sensitivity with 210 – 280 kt.MW.year Discovery ~6-7 years « Genuine potential for early physics discovery 47 04/05/2016 Mark Thomson | DUNE

  29. DUNE Science Summary DUNE physics: • Game-changing program in Neutrino Physics – Definitive 5 σ determination of MH – Probe leptonic CPV – Precisely test 3-flavor oscillation paradigm • Potential for major discoveries in astroparticle physics – Extend sensitivity to nucleon decay – Unique measurements of supernova neutrinos (if one should occur in lifetime of experiment) 48 04/05/2016 Mark Thomson | DUNE

  30. 7. LBNF – a MW-scale facility 8. The DUNE Far Detector 9. The DUNE Near Detector 49 04/05/2016 Mark Thomson | DUNE

  31. 7. LBNF – a MW-scale facility 50 04/05/2016 Mark Thomson | DUNE

  32. LBNF and PIP-II « In beam-based long-baseline neutrino physics: beam power drives the sensitivity § « LBNF: the world’s most intense high-energy ν beam § 1.2 MW from day one • NuMI (MINOS) <400 kW • NuMI (NOVA) 600 - 700 kW § upgradable to 2.4 MW « Requires PIP-II (proton-improvement plan) $0.5B upgrade of FNAL accelerator § infrastructure § Replace existing 400 MeV LINAC with 800 MeV SC LINAC 51 04/05/2016 Mark Thomson | DUNE

  33. The LBNF Neutrino Beam § i) Start with an intense (MW) proton beam from PIP-II § ii) Point towards South Dakota hadrons § iii) Smash high-energy (~80 GeV) protons into a target § iv) Focus positive pions/kaons π + → µ + ν µ § v) Allow them to decay § vi) Absorb remaining charged particles in rock § vii) Left with a “collimated ” beam ν µ p ii) p i) p π iv) iii) v) ν , , µ vi) vii) ν 52 04/05/2016 Mark Thomson | DUNE

  34. The LBNF Neutrino Beam § i) Start with an intense (MW) proton beam from PIP-II § ii) Point towards South Dakota hadrons § iii) Smash high-energy (~80 GeV) protons into a target § iv) Focus positive pions/kaons π + → µ + ν µ § v) Allow them to decay § vi) Absorb remaining charged particles in rock § vii) Left with a “collimated ” beam ν µ p ii) p i) p π iv) iii) v) ν , , µ vi) vii) ν 53 04/05/2016 Mark Thomson | DUNE

  35. 8. The DUNE Far Detector 54 04/05/2016 Mark Thomson | DUNE

  36. Staged Approach to 40 kt Cavern Layout at the Sanford Underground Research Facility based on four independent caverns • Four identical caverns hosting four independent 10-kt FD modules – Allows for staged construction of FD – Gives flexibility for evolution of LArTPC technology design • Assume four identical cryostats • But, assume that the four 10-kt modules will be similar but not necessarily identical #2 #1 #4 #3 55 04/05/2016 Mark Thomson | DUNE

  37. Going underground… DUNE Far Detector site • Sanford Underground Research Facility (SURF), South Dakota • Four caverns on 4850 level (~ 1 mile underground) Ross Campus: Davis Campus: • CASPAR • LUX • … • Majorana demo. • DUNE • … • LZ Green = new excavation commences in 2017 56 04/05/2016 Mark Thomson | DUNE

  38. Far Detector Basics A modular implementation of Single-Phase TPC • Record ionization using three wire planes 3D image E Anode planes Cathode planes − 180 kV e − A C A C A C A ν 12 m 3.6 m wire # wire # wire # 14.4 m time / ms time / ms time / ms Steel Cryostat 57 04/05/2016 Mark Thomson | DUNE

  39. Far Detector Basics A modular implementation of Single-Phase TPC • Record ionization using three wire planes 3D image E Anode planes Cathode planes − 180 kV e − A C A C A C A ν 12 m 3.6 m wire # 14.4 m time / ms Steel Cryostat 58 04/05/2016 Mark Thomson | DUNE

  40. First 17-kt detector Modular implementation of Single-Phase TPC – Active volume: 12m x 14m x 58m – 150 Anode Plane Assemblies • 6m high x 2.3m wide – 200 Cathode Plane Assemblies • Cathode @ -180 kV for 3.5m drift A C A C A Second & subsequent far detector modules S/N ≈ 100 – Not assumed to be exactly the same, could be: • Evolution of single-phase design • Dual-phase readout – potential benefits DP Readout 59 04/05/2016 Mark Thomson | DUNE

  41. Far Detector Development e.g. single-phase APA/CPA LAr-TPC: • Design is already well advanced – evolution from ICARUS • Supported by strong development program at Fermilab – 35-t prototype (run ended 03/2016) tests of basic design 60 04/05/2016 Mark Thomson | DUNE

  42. Far Detector Development e.g. single-phase APA/CPA LAr-TPC: • Design is already well advanced – evolution from ICARUS • Supported by strong development program at Fermilab – 35-t prototype (run ended 03/2016) tests of basic design – MicroBooNE (operational since 2015) – SBND (aiming for operation in 2018) 61 04/05/2016 Mark Thomson | DUNE

  43. Far Detector Development e.g. single-phase APA/CPA LAr-TPC: • Design is already well advanced – evolution from ICARUS • Supported by strong development program at Fermilab – 35-t prototype (run ended 03/2016) tests of basic design – MicroBooNE (operational since 2015) – SBND (aiming for operation in 2018) • 2 “Full-scale” prototype s (protoDUNE) cat the CERN Neutrino Platform – Single-Phase & Dual-Phase – Engineering prototypes, e.g. SP: • 6 full-sized drift cells c.f. 150 in the far det. – Aiming for operation in 2018 62 04/05/2016 Mark Thomson | DUNE

  44. Far Detector Development e.g. single-phase APA/CPA LAr-TPC: • Design is already well advanced – evolution from ICARUS • Supported by strong development program at Fermilab – 35-t prototype (run ended 03/2016) tests of basic design – MicroBooNE (operational since 2015) – SBND (aiming for operation in 2018) • 2 “Full-scale” prototype s (protoDUNE) cat the CERN Neutrino Platform – Single-Phase & Dual-Phase – Engineering prototypes, e.g. SP : • 6 full-sized drift cells c.f. 150 in the far det. – Aiming for operation in 2018 63 04/05/2016 Mark Thomson | DUNE

  45. 9. The DUNE Near Detector 64 04/05/2016 Mark Thomson | DUNE

  46. DUNE ND (in brief) CDR design is the the NOMAD-inspired FGT STT'Module' • It consists of: Barrel' Backward'ECAL' Barrel'' ECAL' RPCs' End' – Central straw-tube tracking system Magnet' RPCs' Coils' – Lead-scintillator sampling ECAL Forward' ECAL' – RPC-based muon tracking systems End' RPCs' • Other options being studied • The Near Detector provides: – Constraints on cross sections and the neutrino flux – A rich self-contained non-oscillation neutrino physics program – N Will result in unprecedented samples of ν interactions – >100 million interactions over a wide range of energies: • strong constraints on systematics • the ND samples will represent a huge scientific opportunity 65 04/05/2016 Mark Thomson | DUNE

  47. 10. Political Context 66 04/05/2016 Mark Thomson | DUNE

  48. Political Context – many firsts « LBNF/DUNE will be: § The first international “mega-science” project hosted by the US • “do for the Neutrinos, what the LHC did for the Higgs” § The first U.S. project run as an international collaboration • Organization follows the LHC model 67 04/05/2016 Mark Thomson | DUNE

  49. Political Context – many firsts « LBNF/DUNE will be: § The first international “mega-science” project hosted by the US • “do for the Neutrinos, what the LHC did for the Higgs” § The first U.S. project run as an international collaboration • Organization follows the LHC model « The U.S. is serious: § LBNF/DUNE is Fermilab’s future flagship project § Very strong support from Fermilab & the U.S. DOE § CD3a in December – funding request for excavation in FY17 currently with DOE 68 04/05/2016 Mark Thomson | DUNE

  50. Political Context – many firsts « LBNF/DUNE will be: § The first international “mega-science” project hosted by the US • “do for the Neutrinos, what the LHC did for the Higgs” § The first U.S. project run as an international collaboration • Organization follows the LHC model « The U.S. is serious: § LBNF/DUNE is Fermilab’s future flagship project § Very strong support from Fermilab & the U.S. DOE § CD3a in December – funding request for excavation in FY17 currently with DOE « A game-changer for CERN and the U.S. § Historic agreement between U.S. and CERN § US contributes to LHC upgrade (high-field magnets) § CERN contributes to Far site infrastructure 69 04/05/2016 Mark Thomson | DUNE

  51. Political Context – many firsts « LBNF/DUNE will be: § The first international “mega-science” project hosted by the US • “do for the Neutrinos, what the LHC did for the Higgs” § The first U.S. project run as an international collaboration • Organization follows the LHC model « The U.S. is serious: § LBNF/DUNE is Fermilab’s future flagship project § Very strong support from Fermilab & the U.S. DOE § CD3a in December – funding request for excavation in FY17 currently with DOE « A game-changer for CERN and the U.S. § Historic agreement between U.S. and CERN § US contributes to LHC upgrade (high-field magnets) § CERN contributes to Far site infrastructure « First truly global neutrino experiment 70 04/05/2016 Mark Thomson | DUNE

  52. Political Context – many firsts « LBNF/DUNE will be: § The first international “mega-science” project hosted by the US • “do for the Neutrinos, what the LHC did for the Higgs” § The first U.S. project run as an international collaboration • Organization follows the LHC model « The U.S. is serious: § LBNF/DUNE is Fermilab’s future flagship project § Very strong support from Fermilab & the U.S. DOE § CD3a in December – funding request for excavation in FY17 currently with DOE « A game-changer for CERN and the U.S. § Historic agreement between U.S. and CERN § US contributes to LHC upgrade (high-field magnets) § CERN contributes to Far site infrastructure « First truly global neutrino experiment 71 04/05/2016 Mark Thomson | DUNE

  53. 11. Opportunities on DUNE 72 04/05/2016 Mark Thomson | DUNE

  54. Opportunities in DUNE DUNE is moving rapidly • Excavation starts in 2017 • ProtoDUNE @ CERN in 2018 • Far Detector construction in 2019 • Far Detector installation in 2021 DUNE: the next large global Particle Physics project • Actively seeking new collaborators – many synergies with collider experiments • Immediate Focus in Europe will be ProtoDUNE @ CERN • Many Opportunities: – Hardware: e.g. photon detection system (scintillator + SiPMs) – DAQ/Computing: continuous readout = high-data rates – Software: LAr-TPC reconstruction 73 04/05/2016 Mark Thomson | DUNE

  55. Opportunities in DUNE DUNE is moving rapidly • Excavation starts in 2017 • ProtoDUNE @ CERN in 2018 • Far Detector construction in 2019 • Far Detector installation in 2021 DUNE: the next large global Particle Physics project • Actively seeking new collaborators – many synergies with collider experiments • Immediate Focus in Europe will be ProtoDUNE @ CERN • Many Opportunities: – Hardware: e.g. photon detection system (scintillator + SiPMs) – DAQ/Computing: continuous readout = high-data rates – Software: LAr-TPC reconstruction 74 04/05/2016 Mark Thomson | DUNE

  56. 12. Summary 75 04/05/2016 Mark Thomson | DUNE

  57. Summary « DUNE will Probe leptonic CPV with unprecedented position § Definitively determine the MH to greater than 5 σ § Test the three-flavor hypothesis § Significantly advance the discovery potential for proton decay § (With luck) provide a wealth of information on Supernova bursts § neutrino physics and astrophysics 76 04/05/2016 Mark Thomson | DUNE

  58. Summary « DUNE will Probe leptonic CPV with unprecedented position § Definitively determine the MH to greater than 5 σ § Test the three-flavor hypothesis § Significantly advance the discovery potential for proton decay § (With luck) provide a wealth of information on Supernova bursts § neutrino physics and astrophysics « This is an exciting time DUNE is now ballistic § The timescales are not long: § DUNE/LBNF aims to start excavation in 2017 • The large-scale DUNE prototype will operate at CERN in 2018 • 77 04/05/2016 Mark Thomson | DUNE

  59. Summary « DUNE will Probe leptonic CPV with unprecedented position § Definitively determine the MH to greater than 5 σ § Test the three-flavor hypothesis § Significantly advance the discovery potential for proton decay § (With luck) provide a wealth of information on Supernova bursts § neutrino physics and astrophysics « This is an exciting time DUNE is now ballistic § The timescales are not long: § DUNE/LBNF aims to start excavation in 2017 • The large-scale DUNE prototype will operate at CERN in 2018 • « An international community is forming – including CERN LBNF/DUNE represents a major new scientific opportunity for § particle physics 78 04/05/2016 Mark Thomson | DUNE

  60. Thank you for your attention 79 04/05/2016 Mark Thomson | DUNE

  61. Backup Slides 80 04/05/2016 Mark Thomson | DUNE

  62. Science 81 04/05/2016 Mark Thomson | DUNE

  63. Parameter Resolutions δ CP & θ 23 • As a function of exposure δ δ Resolution Resolution 2 2 sin sin θ θ Resolution Resolution CP CP 23 23 40 0.04 DUNE Sensitivity DUNE Sensitivity Normal Hierarchy Normal Hierarchy 35 0.035 2 2 sin 2 θ = 0.085 sin 2 = 0.085 θ 13 13 2 2 sin θ = 0.45 sin = 0.45 θ Resolution (degrees) 23 30 23 0.03 Resolution 25 0.025 20 0.02 23 θ 15 0.015 2 sin δ = 90 ° CP CP 10 δ 0.01 5 δ = 0 ° 0.005 CP 0 0 0 200 400 600 800 1000 1200 1400 0 200 400 600 800 1000 1200 1400 Exposure (kt-MW-years) Exposure (kt-MW-years) 82 04/05/2016 Mark Thomson | DUNE

  64. PDK p → K ν • DUNE for various staging assumptions 83 04/05/2016 Mark Thomson | DUNE

  65. Beam Optimization 84 04/05/2016 Mark Thomson | DUNE

  66. Beam Optimization Following LBNO approach, genetic algorithm used to optimize horn design – increase neutrino flux at lower energies 9 Flux, Mode ν ν 10 × µ 80 Optimized, 241x4 m DP Horn 1 / Year 70 Optimized, 195x4 m DP Enhanced Reference, 250x4 m DP Enhanced Reference, 204x6 m DP 60 2 Reference, 204x4 m DP s / GeV / m 50 40 µ ν 30 Unoscillated 20 10 0 0 1 2 3 4 5 6 7 Energy (GeV) ν µ 85 04/05/2016 Mark Thomson | DUNE

  67. Reconstruction 86 04/05/2016 Mark Thomson | DUNE

  68. LAr-TPC Reconstruction Real progress in last year – driven by 35-t & MicroBooNE • Full DUNE simulation/reconstruction now in reach (a) Efficiency of pattern recognition Efficiency of pattern recognition 1 1 5 GeV ν CC 5 GeV ν CC e - 0.8 0.8 µ e 0.6 0.6 " - # 0.4 0.4 0.2 0.2 p 0 0 0 1 2 3 4 5 0 1 2 3 4 5 # True muon momentum (GeV) True electron energy (GeV) 4 GeV e CC 87 04/05/2016 Mark Thomson | DUNE

  69. Schedule 88 04/05/2016 Mark Thomson | DUNE

  70. Indicative schedule Jul-15 Dec-19 CD-1 Refresh CD-2/3c Review Project Baseline/ Construction Approval Preliminary Design CERN Test Final Design and Production Set-up Construction of Detector #1 Components Install Detector #1 Fill & Commission Detector #1 Construction of Detector #2 Components Install Detector #2 Fill & Commission Detector #2 Construction of Detector #3 Components Install Detector #3 Fill & Commission Detector #3 Construction of Detector #4 Components Install Detector #4 Fill & Commission Detector #4 FY15 FY16 FY17 FY18 FY19 FY20 FY21 FY22 FY23 FY24 FY25 FY26 FY27 Cryostat #4 Ready for Start Full Scale Cryostat Cryostat Detector Installation Mockup #2 Ready #1 Ready for Detector Cryostat #3 Ready for for Detector Installation Detector Installation Installation 89 04/05/2016 Mark Thomson | DUNE

  71. Indicative schedule Jul-15 Dec-19 CD-1 Refresh CD-2/3c Review Project Baseline/ Construction Approval Preliminary Design CERN Test Final Design and Production Set-up Construction of Detector #1 Components Install Detector #1 Fill & Commission Detector #1 Construction of Detector #2 Components Install Detector #2 Fill & Commission Detector #2 Construction of Detector #3 Components Install Detector #3 Fill & Commission Detector #3 Construction of Detector #4 Components Install Detector #4 Fill & Commission Detector #4 FY15 FY16 FY17 FY18 FY19 FY20 FY21 FY22 FY23 FY24 FY25 FY26 FY27 Cryostat #4 Ready for Start Full Scale Cryostat Cryostat Detector Installation Mockup #2 Ready #1 Ready for Detector Cryostat #3 Ready for for Detector Installation Detector Installation Installation 90 04/05/2016 Mark Thomson | DUNE

  72. Calculating Sensitivies 91 04/05/2016 Mark Thomson | DUNE

  73. Determining Physics Sensitivities For Conceptual Design Report • Full detector simulation/reconstruction not available – See later in talk for plans • For Far Detector response – Use parameterized single-particle response based on achieved/expected performance (with ICARUS and elsewhere) • Systematic constraints from Near Detector + … – Based on current understanding of cross section/hadro-production uncertainties + Expected constraints from near detector • in part, evaluated using fast Monte Carlo 92 04/05/2016 Mark Thomson | DUNE Oscillation physics with atmospheric neutrinos

  74. Evaluating DUNE Sensitivities I Many inputs calculation (implemented in GLoBeS): • Cross sections • Reference Beam Flux – GENIE 2.8.4 – 80 GeV protons – – CC & NC 204m x 4m He-filled decay – all (anti)neutrino flavors pipe – 1.07 MW Exclusive ν -nucleon cross sections – NuMI-style two horn system • Optimized Beam Flux – Horn system optimized for lower energies • Expected Detector Performance – Based on previous experience (ICARUS, ArgoNEUT, …) 93 04/05/2016 Mark Thomson | DUNE

  75. Evaluating DUNE Sensitivities II • Assumed* Particle response/thresholds – Parameterized detector response for individual final-state particles Particle Threshold Energy/momentum Angular Type (KE) Resolution Resolution 30 MeV Contained: from track length 1 o µ ± Exiting: 30 % 100 MeV MIP-like: from track length π ± Contained π -like track: 5% 1 o Showering/Exiting: 30 % e ± / γ 30 MeV 1 o 2% ⊕ 15 %/√(E/GeV) p 50 MeV p < 400 MeV: 10 % 5 o p > 400 MeV: 5% ⊕ 30%/√(E/GeV) n 50 MeV 440%/√(E/GeV) 5 o other 50 MeV 5 o 5% ⊕ 30%/√(E/GeV) *current assumptions to be addressed by FD Task Force 94 04/05/2016 Mark Thomson | DUNE

  76. Evaluating DUNE Sensitivities III • Efficiencies & Energy Reconstruction – Generate neutrino interactions using GENIE – Fast MC smears response at generated final-state particle level – “Reconstructed” neutrino energy – kNN-based MV technique used for ν e “event selection”, parameterized as efficiencies – Used as inputs to GLoBES CC ν e ν e appearance 95 04/05/2016 Mark Thomson | DUNE

  77. Evaluating DUNE Sensitivities IV • Systematic Uncertainties – Anticipated uncertainties based on MINOS/T2K experience – Supported by preliminary fast simulation studies of ND Source MINOS T2K DUNE ν e ν e ν e Flux after N/F extrapolation 0.3 % 3.2 % 2 % Interaction Model 2.7 % 5.3 % ~ 2 % Energy Scale ( ν µ ) 3.5 % Inc. above (2 %) Energy Scale ( ν e ) 2.7 % 2 % 2 % FiducialVolume 2.4 % 1 % 1 % Total 5.7 % 6.8 % 3.6 % • DUNE goal for ν e appearance < 4 % For sensitivities used: 5 % ⨁ 2 % – – where 5 % is correlated with ν µ & 2 % is uncorrelated ν e only 96 04/05/2016 Mark Thomson | DUNE

  78. 5: Hyper-Kamiokande 97 04/05/2016 Mark Thomson | DUNE

  79. Far Detector Hyper-K is the proposed third generation large water Cherenkov detector in the Kamioka mine Kamiokande Super-Kamiokande Hyper-Kamiokande (1983-1996) (1996-) (202?-) 3 kton 50 kton 1 Mton Inner detector volume = 0.74 Mton § Fiducialvolume = 0.56 Mton § Photomultiplier tubes: 99,000 20” inner detector & 25,000 8” outer detector § 98 04/05/2016 Mark Thomson | DUNE

  80. JPARC Beam for Hyper-K « Upgraded JPARC beam « At least 750 kW expected at start of experiment Physics studies assume 7.5x10 7 MW.s exposure § i.e. 10 years at 750 kW • or 5 years at 1.5 MW • Beam sharing between neutrinos:antineutrinos = 1 : 3 § « Hyper-K is off-axis Narrow-band beam, centered on first oscillation maximum § Baseline = 295 km matter effects are small § 99 04/05/2016 Mark Thomson | DUNE

  81. Hyper-K Science Goals Focus on fundamental open questions in particle physics and astro-particle physics: • 1) Neutrino Oscillations – CPV from J-PARC neutrino beam – Mass Hierarchy from Atmospheric Neutrinos – Solar neutrinos • 2) Search for Proton Decay π 0 – Particularly strong for decays with • 3) Supernova burst physics & astrophysics – Galactic core collapse supernova 100 04/05/2016 Mark Thomson | DUNE

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