1. ISS-2 25 jan. 2006 KEK Alain Blondel ISS-detectors

2. ISS-2 25 jan. 2006 KEK Alain Blondel Water Cerenkov Detectors report by Jacques Bouchez Magnetic Sampling Detectors http://dpnc.unige.ch/users/blondel/detectors/magneticdetector/SMD-web.htm report by Alan Bross Liquid Argon TPC http://www.hep.yorku.ca/menary/ISS/ http://www.hep.yorku.ca/menary/ISS/ reports by Scott Menary, Andreas Badertscher Emulsion Detectors http://people.na.infn.it/~pmiglioz/ISS-ECC-G/ISSMainPage.html http://people.na.infn.it/~pmiglioz/ISS-ECC-G/ISSMainPage.html report by Pasquale Migliozzi Near Detectors http://ppewww.ph.gla.ac.uk/~psoler/ISS/ISS_Near_Detector.html http://ppewww.ph.gla.ac.uk/~psoler/ISS/ISS_Near_Detector.html reports by Paul Soler and Federico Sanchez Working group reports Detector Technology will take place this afternoon

3. ISS-2 25 jan. 2006 KEK Alain Blondel Wednesday 25 January timespeaker 14:00MPPCT. Nakadaira 14 :30SiPMs for T2K ND280 Y. Kudenko 15:00New VLPC R&DA.Bross 15:30Hybrid PMTH. Nakayama 16:00Scintillating Fiber Production (Kuraray) Y. Shiomi 16:30Open discussion Technology discussion session (organized by Alan Bross and Kenji Kaneyuki)

4. ISS-2 25 jan. 2006 KEK Alain Blondel The MEMPHYS Project 65m Fréjus CERN 130km 4800mwe Excavation engineering pre-study has been done for 5 shafts Water Cerenkov modules at Fréjus CERN to Fréjus Neutrino Super-beam and Beta-beam

5. ISS-2 25 jan. 2006 KEK Alain Blondel A Very Large Laboratory In the middle of the Fréjus tunnel at a depth of4800 m.w.e a preliminary investigation shows the feasibility to excavate up to five shafts of about 250,000 m 3 each Henderson HK

6. ISS-2 25 jan. 2006 KEK Alain Blondel 65m ~ 4 x SK 65m Detector basic unit Detector: cylinder (a la SK) 65 m diameter and 65 m height: : → 215 000 tons of water (4 times SK) taking out 4 m from outside for veto and fiducial cut →146 000 ton fiducial target 3 modules : 440 kilotons (like UNO) BASELINE 4 modules would give 580 kilotons (HK) →Simulations done using 440 kt each cavity 70 m diameter and 80 m total height

7. ISS-2 25 jan. 2006 KEK Alain Blondel

8. R&D on electronics (ASICs) Integrated readout : “digital PM (bits out)” Charge measurement (12bits) Time measurement (1ns) Single photoelectron sensitivity High counting rate capability (target 100 MHz) Large area pixellised PM : “PMm 2 ” 16 low cost PMs Centralized ASIC for DAQ Variable gain to have only one HV Multichannel readout Gain adjustment to compensate non uniformity Subsequent versions of OPERA_ROC ASICs aim at 200 euros/channel

9. ISS-2 25 jan. 2006 KEK Alain Blondel Mechanics & PMT tests Basic unit that we want to build and test under water Electronic box water tight IPNO Taken in charge by IPNO: well experienced in photodetectors (last operation: Auger). With PHOTONIS tests of PMT 8”, 9”  12” and Hybrid- PMT and HPD

10. ISS-2 25 jan. 2006 KEK Alain Blondel A possible schedule for MEMPHYS at Frejus Year 2005 2010 2015 2020 Safety tunnel Excavation Lab cavity Excavation P.S Study detector PM R&DPMT production Det.preparation InstallationOutside lab. Non-acc.physics P-decay, SN Superbeam Construction Superbeam betabeam Beta beam Construction decision for cavity digging decision for SPL construction decision for EURISOL site

11. ISS-2 25 jan. 2006 KEK Alain Blondel SUPERBEAM BETABEAM  → e e →   Superbeam + beta beam together 2 ways of testing CP, T and CPT : redundancy and check of systematics 2 beams 1 detector 2yrs 8yrs 5yrs pure4 flavours + K    

12. ISS-2 25 jan. 2006 KEK Alain Blondel MEMPHYS comments (AB) -- French neutrino community strongly motivated -- R&D already started. -- CERN beams (Beta-beam, Superbeam) possible please consider oscillation physics performance with BOTH betabeam gamma=100 AND WBB Superbeam Ep= 3-4 GeV. (no Kaons) ball-park est. cost of total package 600M€ (detector) + + (from erlier est…) betabeam (~500M€) + superbeam (~400 M€) main physics question mark: is it possible at all to do the physics with low energy events ? J. Bouchez promised to investigate the principle of a near detector system to determine cross-sections and efficiencies for the four flavours of neutrinos as function of energy.

13. ISS-2 25 jan. 2006 KEK Alain Blondel

14. considerable noise reduction can be obtained by gas amplification

15. ISS-2 25 jan. 2006 KEK Alain Blondel industrial study of large Tank 70 m diameter, 20 m drift = 100 kton of Larg shown to be feasible conceptually

16. ISS-2 25 jan. 2006 KEK Alain Blondel non- trivial liquid argon consumption!!!!

17. ISS-2 25 jan. 2006 KEK Alain Blondel height is limited by high voltage 1kV/cm  2 MV for 20m… field degrader in liquid argon tested  (Cockroft-Greinacher circuit)

18. ISS-2 25 jan. 2006 KEK Alain Blondel long drift will be tested in 5m vertical drift tube (ETHZ-Napoli) and drift under high pressure in pressurized cryostat

19. ISS-2 25 jan. 2006 KEK Alain Blondel consequences of long drift: time integration 1.Detector must be underground to limit cosmics (are they all just muons?) 2.photomultipliers sensitive to 128 nm scintillation light can be installed for trigger 3.however Raleigh scattering (<1m scattering length) limits position reconstruction from light timing 4.it is possible to tag timing of neutrino events with precision small wrt 100 ns. and operate with both mu+ and mu- trains injected in storage ring

20. ISS-2 25 jan. 2006 KEK Alain Blondel     l l-l- l+l+ ex: race track geometry: constraint: ¦l - - l + ¦ > l +  where  is the precision of the experiments time tag plus margin Muons of both signs circulate in opposite directions in the same ring. The two straight sections point to the same far detector(s). OK There is one inconvenient with this: the fact that there are two decay lines implies two near detectors. In addition this does not work for the triangle. this can be solved by dog bone or two rings with one or more common straights 

21. ISS-2 25 jan. 2006 KEK Alain Blondel

22. NB B field is perp. to drift! NBB: what range of electrons does this correcpond to?

23. ISS-2 25 jan. 2006 KEK Alain Blondel

25. Questions: what is efficiency as a function of energy vs B field? what magnetic field is necessary to have reasonable efficiency for electrons up to first oscillation maximum and a little more? (this is of course a baseline dependent statement) phenomenologists: be prepared to add this to the perfect detector! 10 (100?) kton with 30% efficiency for wrong sign electrons up to 5 GeV ? dreams? High Tc supra conductor magnet?

26. ISS-2 25 jan. 2006 KEK Alain Blondel

27. US Larg effort (Menary) Implementation of Larg detector in Globes underway a few weeks to go!

28. ISS-2 25 jan. 2006 KEK Alain Blondel An ideal detector exploiting a Neutrino Factory should: Identify and measure the charge of the muon (“golden channel”) with high accuracy Identify and measure the charge of the electron with high accuracy (“time reversal of the golden channel”) Identify the  decays (“silver channel”) Measure the complete kinematics of an event in order to increase the signal/back ratio Migliozzi

29. ISS-2 25 jan. 2006 KEK Alain Blondel “MECC” structure Stainless steel or LeadFilmRohacell DONUT/OPERA type target + Emulsion spectrometer + TT + Electron/pi discriminator B Assumption: accuracy of film by film alignment = 10 micron (conservative) 13 lead plates (~2.5 X 0 ) + 4 spacers (2 cm gap) (NB in the future we plan to study stainless steel as well. May be it will be the baseline solution: lighter target) The geometry of the MECC is being optimized 3 cm Electronic detectors/ECC

30. ISS-2 25 jan. 2006 KEK Alain Blondel Momentum resolution for muons

31. ISS-2 25 jan. 2006 KEK Alain Blondel Charge misidentification

32. ISS-2 25 jan. 2006 KEK Alain Blondel Estimate of showering electrons

33. ISS-2 25 jan. 2006 KEK Alain Blondel Momentum resolution vs z vertex

34. ISS-2 25 jan. 2006 KEK Alain Blondel q-mis vs z vertex Given the true-hit based reconstruction, the quoted charge misidentification can be seen as an lower limit. Anyhow it is a good starting point! the real question will be how many right signs appear as wrong sign!

35. ISS-2 25 jan. 2006 KEK Alain Blondel Migliozzi

36. ISS-2 25 jan. 2006 KEK Alain Blondel segmented magnetic detector (Bross)

37. ISS-2 25 jan. 2006 KEK Alain Blondel

38. Muon 3 GeV/c

39. ISS-2 25 jan. 2006 KEK Alain Blondel Electron

40. ISS-2 25 jan. 2006 KEK Alain Blondel Momentum Resolution

41. ISS-2 25 jan. 2006 KEK Alain Blondel

42. 3. Flux normalisation (cont.) o Rates: — E  = 50 GeV — L = 100 m, d = 30 m — Muon decays per year: 10 20 — Divergence = 0.1 m  /E  — Radius R=50 cm 100 m Yearly event rates High granularity in inner region that subtends to far detector. E.g. at 25 GeV, number neutrino interactions per year is: 20 x 10 6 per 100 g/cm 2. With 50 kg  10 9 interactions/yr

43. ISS-2 25 jan. 2006 KEK Alain Blondel 3. Flux normalisation (cont.) o Neutrino flux normalisation by measuring: o Signal: low angle forward going muon with no recoil o Calculable with high precision in SM o Same type of detector needed for elastic scattering on electrons: E.g. CHARM II obtained value of sin 2  W from this

44. ISS-2 25 jan. 2006 KEK Alain Blondel 4. Muon polarization o Fit neutrino spectrum for polarization: Compare fitted polarization to measured one from polarimeter:

45. ISS-2 25 jan. 2006 KEK Alain Blondel 5. Cross sections o Measurement of cross sections in DIS, QE and RES.  Coherent  o Different nuclear targets: H 2, D 2 o Nuclear effects, nuclear shadowing, reinteractions o With modest size targets can obtain very large statistics o What is lowest energy we can achieve? E.g. with LAr can go down to ~MeV

46. ISS-2 25 jan. 2006 KEK Alain Blondel

48. threshold will be different for e and mu, affected by fermi motion, reinteractions and Q2 distribution (neutrino  antineutrino)

49. ISS-2 25 jan. 2006 KEK Alain Blondel

51. 6. Charm Production o Remember that main background to golden channel is production of charm:  Q t = P  sin 2  cut eliminates backg at 10 -6 not detected NC CC Hadron decay o Can use near detector to measure Pt and Qt distribution of charm, if we can reconstruct explicitly: o With silicon detector can reconstruct more than 10 6 charm states per year Cervera et al.

52. ISS-2 25 jan. 2006 KEK Alain Blondel 6. Charm (cont.) o NOMAD-STAR silicon detector was able to reconstruct 45 charm events in NOMAD. o Measured charm rate:  Fully active silicon target (ie. 52 kg with 18 layers of Si 500  m thick, 50 x 50 cm 2 =4.5 m 2 ) for full charm event reconstruction. o Optimal design: fully pixelated detector (e.g. Monolithic Active Pixels MAPS)

53. ISS-2 25 jan. 2006 KEK Alain Blondel Next steps 0. everyone to produce web site and mailing list 1. develop simulation of detector with justified level of simplification for performance evaluation. (no need to have full simulation to evaluate charm decays in flight!) 2. develop tool to evaluate performance: GLOBES input files in form of eficiency for neutrino type  to be detected as event class i   i  E , P , Q T ) (NB limitation is that all types and classes must have same energy binning) 3. begin to think of R&D developments and experiments to be performed, (preferably on real neutrino physics experiments) 4. cost model mass term + B-field term + 3 sigma charge confusion at 1.5 GeV muon or 6 GeV electron 5. delegate one rep/group to the physics meeting in Boston

54. ISS-2 25 jan. 2006 KEK Alain Blondel 7X7 table for each Ev, y, (x?)

55. ISS-2 25 jan. 2006 KEK Alain Blondel near detector Set-up a generic simulation of a near detector Define a series of potential detector geometries to run on near detector -- dedicated purely-leptonic detector for absolute fluy -- quasi-elastic, pi, pi0 detector with variable targets (a la T2K ND280) -- charm detector for Nufact Carry out physics studies needed for the ISS report: 1.Study flux normalisation through: 2.Use quasi-elastic and elastic interactions to determine neutrino spectrum 3.Reconstruct muon polarization from spectrum 4.Sensitivity for cross-section measurements: low energy? 5.Determination of charm: remember this is main background for golden channel! 6.….suggestions ….

56. ISS-2 25 jan. 2006 KEK Alain Blondel ISS- detector video conferences 14:00 GMT 23 february 16 march 13 april Detector group will delegate 1 person per sub-group to physics meeting in Boston already known to be invited for next meeting at RAL Juha Peltoniemi: (Oulu Mine) Jan Sobczyk: (Wroclaw –theorist- low energy interactions) Introduction: Pasquale Migliozzi Summary: Paul Soler THANKS to ALL!