Hyper-Kamiokande R&D. Francesca Di Lodovico (QMUL) on behalf of the Hyper-Kamiokande working groups

Transcription

1 Hyper-Kamiokande R&D Francesca Di Lodovico (QMUL) on behalf of the Hyper-Kamiokande working groups NNN13, Kavli, IPMU November 013

2 The Hyper-Kamiokande Project Multi-purpose neutrino experiment. Main goal: CP violation Supernova Neutrino oscillations, using both: Neutrino beam from J-PARC (expected beam > 1MW) Sun Accelerator (J-PARC) Atmospheric neutrinos Search for proton decay Solar neutrinos Astrophysical neutrinos (supernova, dark matter, solar flare,...) Neutrino geophysics Proton decay

3 Hyper-Kamiokande Overview 5 x Super-Kamiokande 3

4 Hyper-Kamiokande Overview Water Cherenkov, proved technology & scalability: Excellent PID at sub-gev region >99% Large mass statistics always critical for any measurements. Total Volume 0.99 Megaton Inner Volume 0.74 Mton Fiducial Volume 0.56 Mton (0.056 Mton 10 compartments) Outer Volume 0.0 Mton Photo-sensors 99,000 0 Φ PMTs for Inner Detector (ID) (0% photo-coverage) 5,000 8 Φ PMTs for Outer Detector (OD) Tanks tanks, with egg-shape cross section 48m (w) 50m (t) 50 m (l) 5 x Super-Kamiokande 4

5 Outline Physics in a nutshell Letter of Intent, Hyper-K WG arxiv: [hep-ex] and updates R&D Software (Beam &) Near Detectors Cavern Construction Detector Design PMTs Others Schedule and Summary 5

6 Physics in a Nutshell

7 Tokai--Hyper-Kamiokande Hyper-Kamiokande Natural extension of the technique being proven by the success of TK: Use J-PARC beam Hyper-K at 95km as Super-K Off-axis narrow-band beam E ~0.6 GeV Expected Unoscillated Neutrino Flux at Hyper-K 7

8 Expected Sensitivity to CP Violation CPV discovery sensitivity w/ mass hierarchy known. precision: < 10 for =0 (< 0 for =90 ) Assuming 5% nominal systematics and 0.750MW/y (3y beam and 7y -beam), 74% region of can be covered at 3 It corresponds to a precision of < 10 for =0. 8

9 Using Atmospherics Sensitivity mainly depends on 3,, and MH. 3 mass hierarchy determination for sin 3 > 0.4 (0.43) for normal (inverted) hierarchy (10y). Caveat: the method to determine is used. Ongoing work to use Qian et al., PRD 86, (01). Beam Map Atm. ν Map Add Atm. ν + Beam Hierarchy is unknown, but NH is true. True CP = 0.0; sin 13 = 0.10; sin 3 = 1.0 Degenerate solution exists at 3 for the beam-only case. 9

10 Proton Decay Sensitivities Surpass SK limit in ~1 year year 10 times better sensitivity than Super-K Hyper-K surpasses SK limits in ~1y p e 0 : y at 90%CL p K+: y at 90%CL Many other modes: (p,n) (e, ) + (,, ) K0 modes 0, +. 5y 10

11 Other Physics Topics at Hyper-K Solar Neutrinos: 00 ν s / day from Sun study of day/night asymmetry of the solar neutrinos flux. Astrophysical neutrinos: ~00k ν s from Supernova at Galactic center (10kpc) time variation & energy can be measured with high statistics For supernova explosions outside our galaxy, we expect ~30-50 events from M31 (Andromeda Galaxy) We expect ~310 SRN in the energy range ~30-50 MeV for 10y. Solar flare neutrinos can be detected by Hyper-K and will be a strong test of neutrino emission models. Indirect dark matter search. Geophysical neutrinos measurement of Earth's density. 11

12 R&D Software (Beam &) Near Detectors Cavern Construction Detector Design PMTs Others

13 WCSim WCSim is a flexibile Geant4-based simulation of a water-cherenkov detector with top and side photo-multiplier tubes. Developed by Duke University: Implemented Hyper-Kamiokande egg-shape geometry (WCSim default: cylinder shape). Nominal Cylindrical Geometry Hyper-K egg-shape Implementation of Hyper-K egg-shape 13

14 WCSim WCSim is a flexibile Geant4-based simulation of a water-cherenkov detector with top and side photo-multiplier tubes. Developed by Duke University: Implemented Hyper-Kamiokande egg-shape geometry (WCSim default: cylinder shape). e- 600MeV/c µ- 600MeV/c Ongoing work to develop software and more in general computing model for Hyper-K to be used in future physics studies. 14

15 (Beam &) Near Detectors Super-Kamiokande Hyper-Kamiokande 95 km February, (Tokai)

16 Beam for Tokai--Hyper-Kamiokande Next upgrade (intermediate plan) towards a 750kW operation. See T. Sekigushi's talk for details on the upgrade. It will concern: Upgrade plan for J-PARC accelerators. Upgrade plan for the neutrino beam-line to accept a 750MW beam. 16

17 Near Detectors Currently two near detectors: INGRID, on-axis, for neutrino beam direction. ND80, off-axis, for spectrum measurement. TK Summer 013 e appearance measurement. Predicted number of events error reduction due to ND80: Ongoing discussion on ND80 possible upgrade for HyperKamiokande (THK). 17

18 Near Detector(s) New Near Detector(s) current under-investigation. Several options. Reduce the current systematic errors at Hyper-Kamiokande using: ND beam spectrum similar to HK spectrum same WC detector as Hyper-K 0 xsection measurement, good - separation,.. e e Energy spectrometer energy spectrometer ~1kton km Xsection view WC WC Muon Range Detector Inspired by 007 km TK proposal Poster #0, M. Hartz, M. Wilking 18

19 Cavern Construction

20 HK Technical Design Document Candidate Site: Tochibora Mine Located under Nijugo-yama (Mt. 5), ~8km south from Super-K. Identical baseline (95km) and off-axis angle (.5º) to TK. Overburden ~650m (~1755 m.w.e.). Nijugo-yama The candidate site vicinity was used for mining. Historically many surveys have been done in wide area and at several levels/depths, ex. mapping the location of faults. Many existing tunnels and shafts already escavated. 0

21 Geological Survey The rock mass characterization has been done by mapping the existing tunnels and geological logging of rock core samples. South-side Cavern North-side Cavern 1

22 Rock Mass Characterization From the survey results, rock mass characteristics are classified into 6 categories: A, B, CH, CM, CL and D (defined by CRIEPI). A (blue) is the highest grade rock and D (red) is lowest. Based on these results, HK tank location decided. (CRIEPI: The Central Research Institute of Electric Power Industry) HK tank location For both caverns for the tank locations, 90% of bedrock is CH or higher grade.

23 Cavern Stability Initial stress measurements Plasticity region depth PS-anchor tension CH class (>70% at HK location) 5m 13m CM class (0~30% at HK location) Segmented wall surface of caverns Based on the survey results (rock mass characteristics and initial stresses), the structural stability of caverns was studied The excavation-steps were taken into account in the studies, including the cavern supporting material. For all rock mass classes (B, CH, CM), HK caverns can be constructed by existing excavation/support techniques. 3

24 Excavation Schedule Tunnel constructions Cavern excavation Cavern construction period: ~5 years Transport / approach tunnels: ~3 years Excavation of caverns: ~3 years 4

25 H-K Tanaka Geological Survey at Mozumi Mine Geological survey at the Mozumi mine, already used for Super-K, recently started. It should allow to have deeper caverns (> 700m overburden). First rock mass characterization has been done: rock quality at Mozumi-site is comparable with Tochibora-site More tests under way to complete the geological survey. 5

26 Detector Design

27 Hyper-K Tanks Fiducial volume Inner Detector Two water tanks: 54m(H) x 48m(W) x 50m(L) / tank Water tanks are segmented into 10 compartments 5 compartments / tank Each compartment optically separated and consists of Inner Detector (ID) and Outer Detector (OD) 7

28 Water Containment System Tank lining consists of concrete (60cm) and Polyethylene (5mm) linings welded Polyethylene sheet Drain lines are separated for sump water and leak-water from tank. Drain pipe (for leak water from tank) Drain pipes (for sump water) HDPE lining Concrete lining Waterproof sheet Shotcrete Rock 8

29 Photo-sensor Support Number of photo-sensors: Inner Detector (ID): ~99,000 of 0 (0% photo coverage) Outer Detector (OD): ~5,000 of 8 (identical coverage to SK) Stainless-steel supporting structure holds photo-sensors Inner PMT (0 ) Barrel part Segmentation wall Mounting Photo-sensor Housing 9 9

30 Designing work... The major part of HK tank has been designed. Include layout of water pipes, front-end electronics, cables, calibration holes, plug manholes,... etc. Water piping layout Electronics & cable layout Photo-sensor housing : Inner top pipe : Inner barrel pipe : Inner bottom pipe : Outer top pipe : Outer barrel pipe : Outer bottom pipe : Inlet/Outlet 3960mm 5940mm Calibration holes Plug manhole : Support structure : Cable for inner PMT : Cable for outer PMT : Network/Power cable : Hub / Front End Electronics : Inner photo-sensor (0 ) : Outer photo-sensor (8 ) 30

31 Tank construction schedule Cavern Tank 1 year Lining PMT & support Tank construction: ~ years Lining: 1+ years, PMT installation: ~1 year 31

32 Hyper-K photo-sensor working group See F. Retiere's talk for details on types of HK photosensors 8'' HPD Testing 0ns Integrated Charge Distribution 90ns 8mV 1 p.e. 1p.e. Pedestal p.e. 3p.e. P/V ratio ~4 (~1.7 for 0 PMTs) 1 p.e. 1.ns σ Waveform from HPD output Peak Valley Pre-test performed before installation in a 00ton tank. Confirmed that the basic performance was good P/V: ~4, TTS: ~1ns, Dark rate: comparable to 0 PMTs, 3

33 Tests in a Water Cherenkov Detector EGADS detector : a 00 ton scale model of Super-K To demonstrate the safety and effectiveness of SK + Gadolinium 40 inward-facing photodetectors Electronics : ATMs (used in SK-1,,3), to be upgraded to QBEEs (SK4) Eight 8 HPDs and five 0 high-qe PMTs were mounted Other 7 photodetectors are R3600, and can be used as references for the new photodetector evaluation EGADS 00t tank ~7m 8 HPDs 0 high-qe PMTs 33

34 Photodector Installation in EGADS HPD with supporting frame All 40 photodetectors were installed in July-August 0 High-QE PMT Water-proof cable connection 8 HPD Cable connection in the tank 34

35 Testing in EGADS: Multi p.e.s peaks by HPDs EGADS is in the commissioning phase Initial tests with new photosensors started. Output linearity 500 Charge [pc] p.e. 000 p.e.s p.e.s p.e.s χ / ndf 1.3 / p ± p1 3.7 ± Charge [pc] 4 5 Peak resolution Peak resolution [σ] Multi photoelectron peaks are clearly visible. About 30% σ at 1 p.e. peak 3 Number of photoelectrons χ / ndf / Prob p ± p ± Number of Photoelectrons 35

36 Future Tests Hamamatsu Photonics K.K. is making prototypes of New 0 PMT (Box&Line dynode) 0 HPD Planning to start tests in this year Future: continue tests at different facilities: EGADS 1kton WC prototype (construction ) Other facilities (KEK, Kashiwa, TRIUMF,...) 36

37 Other R&D Water system Readout electronics Calibration system DAQ... Progress within the international working group 37

38 Schedule & Summary

39 Overall Project Schedule Overall Hyper-K construction: ~7 years 39

40 The Hyper-Kamiokande Project Three International Open Meetings (01-013) so far. Formed international working groups. August 1-3, 01 June 1-, January 14-15, Next meeting: 7-8 January 014, Kavli, IPMU. First EU Open Meeting 18 December 013, London 40

41 Summary Hyper-K covers wide range of physics: Neutrino oscillation with beam-ν & atmospheric-ν Main goal: CP violation Nucleon decay search and astrophysical neutrinos R&D started in all areas and progressing: - Software - (Beam &) Near Detectors - Cavern Construction (technical design document ready) - Detector Design - PMTs - Others (electronics, DAQ, water system, calibration, etc.) Japan HEP community: HK at highest priority. Strongly growing international community. Next Hyper-K Open Meeting: January 7-8, Kavli, IPMU. 41

42 Backup Slides

43 e Probability Cij =cos θij, S ij =sin θ ij Φ=Δ mij L 4 Eν Leading term 13 +8C13 S 1 S 13 (C 1 C 13 cos δ S 1 S13 S 3 )cos Φ 3 sin Φ 3 sin Φ1 CPC CPV P( νμ ν e)=4c13 S 13 S3 sin Φ 31 8C13 C 1 C 3 S1 S 13 S 3 sin δ sin Φ3 sin Φ 31 sin Φ for P( e) + 4S C (C C + S S S C1 C 3 S 1 S 3 S 13 cos δ)sin Φ 1 al 8C13 S1 S 3 (1 S13 )cos Φ 3 sin Φ31 4 Eν a +8C13 S 13 S3 (1 S )sin Φ31 13 Δ m13 a= G Solar Matter Effect 5 F ne E= ev ρ E 3 gcm GeV Leading Term sin 13 CPV Term sin 13 Matter Effect sin 13 For large sin 13: Signal, CP Asymmetry, Matter/CP 43

44 e Probability Cij =cos θij, S ij =sin θ ij Φ=Δ mij L 4 Eν Leading term 13 +8C13 S 1 S 13 (C 1 C 13 cos δ S 1 S13 S 3 )cos Φ 3 sin Φ 3 sin Φ1 CPC CPV P( νμ ν e)=4c13 S 13 S3 sin Φ 31 8C13 C 1 C 3 S1 S 13 S 3 sin δ sin Φ3 sin Φ 31 sin Φ S C (C C + S S S C1 C 3 S 1 S 3 S 13 cos δ)sin Φ 1 al 8C13 S1 S 3 (1 S13 )cos Φ 3 sin Φ31 4 Eν a +8C13 S 13 S3 (1 S )sin Φ31 13 Δ m13 a= G Comparison between P( e) and P( e): - for P( e) Solar Matter Effect 5 F ne E= ev ρ E 3 gcm GeV Difference P( e) and P( e) as large as ~±5% at nominal (δ=0) 44

45 Simulated e Candidates after Selection Full simulation of beam, detector response and reconstruction PMT Coverage: ~0% ~000 ~ 3600 events in and beams, respectively Major backgrounds: beam e/ e and NC- 0 45

46 Neutrino Energy Distribution: Effect of 0.75MW 3y 0.75MW 7y =½ = = 3/ Difference from =0: Number + shape sensitive to all values of 46

47 Expected Sensitivity to CP Violation Fractional region of for which the CPV (sin 0) significance is > 3 5% systematics on signal, BG, e BG, / 47

48 Atmospheric Neutrinos e appearance and distortion are expected due to the MSW effect in the Earth's matter: Mass hierarchy: asymmetry between neutrinos and antineutrinos Octant of oscillation: appearance (and disappearance) interplay CP phase (and 13):magnitude of resonance effect. P(νµ νe) Interference Solar Term Matter Sub-GeV Φ (ν e ) Solar Term 1 P (r cos θ 3 1) Φ0 (ν e ) r sin θ 13 cos θ 13 sin θ 3 (cos δ R sin δ I ) + sin θ 13 (r sin θ3 1) P=P (ν e ν μ, τ ) Multi-GeV Interference Matter Effect R and I are the oscillation amplitudes for CP even and odd terms 48

49 Oscillated e flux relative to the non-oscillated flux as a function of the neutrino energy for the up-ward going neutrinos with zenith angle 0.8 Through matter effect (MSW), we study: Mass Hierarchy: asymmetry between and Octant of 3: e appearance and disappearance interplay CP (and 13): magnitude of resonance effect 49

50 Mass Hierarchy Sensitivity 10 years Multi-GeV νe-like events Multi-GeV νe-like events Sensitivity mainly depends on 3, Also some dependence on the mass hierarchy. 3 mass hierarchy determination for sin 3 > 0.4 (0.43) for normal (inverted) hierarchy for 10y data taking. Caveat: the method to determine the number of 's is used. 50

51 Sensitivity to δcp and θ13 (No Reactor Constraint, NH) sinθ13 = 0.10 σινθ3 = 0.50 sinθ13 = 0.10 σινθ3 = 0.50 µ3 =.4ξ10 3 ες µ3 =.4ξ10 3 ες δχπ = (40 δεγ ) δχπ = ( 40 δεγ )

52 Sensitivity to δcp and θ13 (No Reactor Constraint, NH) sinθ13 = 0.10 sinθ3 = 0.50 m3 =.4x10-3 ev δcp =.443 (140 deg ) sinθ13 = 0.10 sinθ3 = 0.50 m3 =.4x10-3 ev δcp =.443 ( 140 deg )

53 Atmospheric Neutrino Sensitivity Summary Objective Hierarchy Octant Normal Inverted Comment σ sinθ3 > 0.96 sinθ3 > σ sinθ3 > 0.4 sinθ3 > 0.4 σ sinθ3 > sinθ3 > years 3σ sinθ3 > 0.99 sinθ3 > years 5 years 10 years 53

54 Sensitivity for 3 Octant and CPV 3 octant sensitivity. Thickness of the band corresponds to the uncertainty from CP. sin 13 = sin 13 = θ13 is fixed : sinθ13 = NH IH Excluded 3 CP fraction. Sensitivity to CP-violation is limited under both hierarchy assumptions. 54

55 Nucleon Decays Only direct probe of Grand Unified Theories Many GUT models predict decays of protons and bound neutrons with = O( ) years. Two modes favoured by many models: p e+ 0 Other modes are also important. p k+ 55

56 Experimental Limits Most stringent limits from Super-K for many decay modes. No signal evidence has been found give constraints on models. After 15y Super-K running (0kton years): (p e+ 0)> y (p k+) > Order of magnitude necessary to be significant. 56