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THE AMS RICH COUNTER

THE AMS RICH COUNTER. AMS. M. Buénerd ISN Grenoble. Plan AMS project RICH counter Prototype. The AMS RICH collaboration: Bologna, Grenoble, Lisbon, Madrid, Maryland, Mexico. The AMS collaboration. UNAM. S.C.C. TING (MIT), PI. AMS Scientific Program on the ISS.

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THE AMS RICH COUNTER

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  1. THE AMS RICH COUNTER AMS M. Buénerd ISN Grenoble • Plan • AMS project • RICH counter • Prototype RICH2002@Pylos The AMS RICH collaboration: Bologna, Grenoble, Lisbon, Madrid, Maryland, Mexico

  2. The AMS collaboration UNAM S.C.C. TING (MIT), PI RICH2002@Pylos

  3. AMS Scientific Program on the ISS • High statistics study of Cosmic Ray particles: • Allowing sensitive search for : • Primordial antimatter(primary goal of the project): • Dark matter (neutralino annihilation): • High energy gamma ray astronomy RICH2002@Pylos

  4. The AMS & RICH calendar • 1994 Approval of the project by NASA/DOE • June 1998:Instrumental flight on the space shuttle DISCOVERY, 10 days • 1999-2004:AMS02 design & construction for ISS phase: SC magnet+ECAL+RICH+TRD • 2005: AMS02 launch & installation on the International Space Station • ~2005-2008: Data taking RICH2002@Pylos

  5. TRDe+/p & e-/p Discrim P<300GeV/c - THE AMS SPECTROMETER TOF Hodoscopes(TOF & dE/dX) Cryostat & SC Magnet(B = 1T) VETO Tracker(P & dE/dX measurement) RICH(particle ID A<~25, Z<~25) EMC(ID em particles) RICH2002@Pylos

  6. Rôle in AMS: • Ion identification (A & Z) • p/e- and p/e+ discrimination • Albedo particle rejection _ THE AMS RICH COUNTER RICH2002@Pylos

  7. RICH design history • 1997-99 : - First simulation works to evaluate the possible performances: see NIM A454(2000)476 • - Study prototype, construction and operation(T.Thuillier et al., NIM A, in press, astro-ph/0201051) • 2000-2002 : - (Iterations to) final design • - Second generation prototype RICH2002@Pylos

  8. è • Proximity focusing counter, photomultipliers • 2 radiators for a maximum momentum range for particle identification (~1-13 GeV/c/nucleon) Imaging technique & main design features • Design drastically constrained by: • Volume • Weight (currently ~190kg) • Power consumption • Long term reliability of components • Magnetic field in the photodetector region RICH2002@Pylos

  9. Simulation of 10Be detection 10Be 9Be 7Be A.Bouchet et al,Nucl.Phys A668(2000) The isotopic abundance ratio 10Be/ 9Be depends on: - Time of confinement of CRs in galaxy - ISM density and galactic halo size 6 weeks counting è ~ 200000 events ! RICH2002@Pylos

  10. The RICH architecture ECAL hole Radiator(s) Conical mirror Photodetectors RICH2002@Pylos

  11. Rich assembly (exploded view) Mirror made inUSA (~13kg) Resp. Bologna NaF radiator ? AEROGEL radiatorplane. Produced in Japan, Characterized in Mexico Support structure Madrid Photon drift space Photodetector plane 680 PMTs ~104 pixels of photosensors(Japan) Mech Designfrom GavazziCo, Italy Structure Assembly (Bologna/Gavazzi) LOWER PANEL RICH2002@Pylos

  12. Shielding Grid Structure Courtesy G. Sardo, Gavazzi Space Co End beam Th. = 0.8 mm Th. = 1.0 mmTh. = 1.2 mm Support beam Bottom skin RICH2002@Pylos

  13. Photomultipliers • Requirements: • Must stand high magnetic field (>~100 G) • Multianode ~5x5mm pixels è Hamamatsu R7600-M16 RICH2002@Pylos

  14. RICH photodetector and front end electronics assembly PMT HamamatsuR7600-M1616 anodes~4.5x4.5mm2 PC Boards, RO and HVD Flex(ible) support Integrated Circuit: AustriaMikroSystem Technology RICH2002@Pylos

  15. Front end electronics Principle: Spectroscopy type charge preamplifier, 16 multiplexed channels, 2 gain (x1 & x5) modes RICH2002@Pylos

  16. Prototype of detector module (16) Light guides (16 pixel) PMT Readout electronics Housing (half) shell RICH2002@Pylos

  17. RICH prototype (2nd generation) RICH2002@Pylos

  18. Prototype = ~½ module of final counter Rich detector plane Prototype a96 PMTs, 1536 pixels RICH2002@Pylos

  19. Prototype experimental set-up (Cosmic ray configuration) Cosmic m Scintillators Trigger electronics and MWPC readout MWPCs Vacuum chamber Radiator PMT Matrix AMS Proto DAQ 3 Radiators tested aerogels 1.03, 1.05, NaF RICH2002@Pylos

  20. Detection plane PMT array before light guide Installation Light guides installed RICH2002@Pylos

  21. Back view of proto 2 Readout lines(9 PMTs/line) RICH2002@Pylos

  22. Top view of the set-up LED PMT matrix Scintillators RO electronics MWPC tracker Vacuum chamber Chamber lid RICH2002@Pylos

  23. PC2 RICH prototype DAQ setup Tracker : MWPCs + delay line RO [CAMAC] Trigger : scintillators + PMTs [CAMAC] P S VME BUS SUN Station RICH2002@Pylos L. Gallin-Martel ISN Grenoble, AMS - CERN October 19th 2001

  24. Readout and DAQ • Each board (33PMTs): • 1 DSP controlled FPGA + memory buffer • 3 DAQ modes controlled by DSP: • calibration: pedestal calibrated and tabulated • RAW: 2 gains and all channels stored • REDUCED : gain mode selection and channel reduction RICH2002@Pylos

  25. Particle hit on LG+PMT Prototype performances in Cosmic Ray tests Example of (muon) event measured in CR tests RICH2002@Pylos

  26. Velocity resolution Only a resolution estimate since no measurement of the incident momentum of particles. Reconstructed b spectrum Aerogel radiator n=1.03 ° Data • Resolution per hit: • Measured: 3.2 10-3 • MC : 2.5 10-3 MC simulation è (Db/b)event~ 10-3 (Z=1) Contribution from mwpc tracker being reduced RICH2002@Pylos

  27. Next steps • Technical tests : Vacuum, thermal, vibrations • Ion beam test at CERN on next october • Detector modules assembly will start on next January 2003. • - Counter assembly finalized by end of 2003. RICH2002@Pylos

  28. Summary & Conclusion • The AMS RICH is fully designed • End-to-end tests of the prototypes have been performed successfully. • Radiators (aerogels 1.03/05, NaF), PMTs, Light guides, FE and RO electronics, processing algorithms, provide the expected results (See talk by F. Barao). • The forthcoming in-beam tests with ions at CERN on october will complete the tests. • è The AMS RICH is on the tracks…. for flying on the ISS. RICH2002@Pylos

  29. Cosmic Ray studies with the RICH What the RICH will do: • Reject Albedo particles (prototype inefficiency < 10-3 ) • Discriminate e+/p & e-/pbar (p < ~12 GeV/c) • Identify nuclei or elements: Assuming DP/P~1% RICH2002@Pylos

  30. <G(x5)> = 69<s/Q> ~ 0.47 <sped> ~ 4.3 Electronics settings PMTs grouped by 11 (10) / flex RICH2002@Pylos

  31. Raw data vs simulation RICH2002@Pylos

  32. Noise 3 ms delayed trigger Aerogel 1.03 run El noise ~ 8 10-5 hit/chan DC ~ 4 10-5 hit/chan RICH2002@Pylos

  33. Proto_1 Z separation Z separation obtainedwith proto 1 at GSI with 1GeV/n 12C beam RICH2002@Pylos

  34. Proto_1 b(z) resolution bresolution obtainedwith proto 1 at GSI with 1GeV/n 12C beam. RICH2002@Pylos

  35. Field map at PMTs RICH2002@Pylos

  36. What ion mass and charge ID range with the RICH ? • From simulation results: • Mass range A< ~30 • Charge range Z< ~25 • Momentum range P< ~15 GeV/c Assuming DP/P~1% The upper bounds quoted for A and Z are asymptotic limits RICH2002@Pylos

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