ic genti

Slide1: 

The Alpha Magnetic Spectrometer on the International Space Station Simonetta Gentile Università di Roma La Sapienza, INFN ICRC03, Tsukuba, Japan

Slide4: 

International Collaboration ~200 scientists + dozens of contractors U. of Aarhus (DK); Academia Sinica (Taiwan); U. of Bucharest (RO); Chinese Academy of Sciences, Inst. of High Energy Physics IHEP (Beijing); Chinese Academy of Sciences, Inst. of Electrical Engineering IEE (Beijing); Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas CIEMAT (Madrid, ES); Chung Shan Inst. of Science and Technology CSIST (Taiwan); EHWA Women's University (Seoul, KR) ETH Zurich (CH); Florida A&M U. (Tallahassee, FL); U. of Geneva (CH); Helsinki U. of Technology (FI); INFN Bologna & U. Bologna (IT); INFN Milano (IT); INFN Perugia, (IT); & U. Perugia (IT); INFN Pisa & U. Pisa (IT); INFN Roma & U. Roma (IT); INFN Siena & U Siena (IT); Inst. Superior Technico (Lisbon, PT); Inst. di Ricerca sulle Onde Elettromagnetiche IROE (Florence, IT); Inst. des Sciences Nucleaires de Grenoble ISN (FR); Inst. for Theoretical and Experimental Physics ITEP (Moscow, RU), Jiao Tong U. (Shanghai); Johns Hopkins U. (Baltimore, US); U. of Karlsruhe (DE); Kurchatov Institute (Moscow, RU); Kyungpook National University CHEP (Taegu, KR); Laboratoire d'Annecy-le-Vieux de Physique des Particules LAPP (FR); Laboratório de Instrumentaço e Física Experimental de Partículas LIP (Lisbon, PT); U. Maryland (College Park, US); Max Planck Inst. (Garching, DE) ; Massachusetts Inst. of Technology MIT (Cambridge, US); U. Montpellier (FR); Moscow State University (RU), Nat'l Aerospace Laboratory NRL (Amsterdam, NL); U. Nacional Autonoma de Mexico (MX); Nat'l Space Program Office (Taiwan); Nat'l Central University NCU (Taiwan); Nat'l Inst. for Nuclear Physics and High Energy Physics NIKHEF (Amsterdam, NL) I. Physikalisches Inst., RWTH Aachen (DE); III. Physikalisches Inst., RWTH Aachen (DE); Southeast U. (Nanjing); U. of Turku (FI); Yale U. (New Haven, US); Lockheed Martin, USA; Space Cryomagnetics LTD, UK; Arde, Inc., USA; CAEN Aerospace, IT; Carlo Gavazzi Space SpA, IT; ISATECH Engineering GmbH, DE; OHB GmbH, DE; Linde; NASA

Slide5: 

Transition Radiation Detector Time of Flight scintillator counters 8 layers of Si strip tracker planes in superconducting magnet Rich Imaging Cerenkov detector Electromagnetic calorimeter

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The Alpha Magnetic Spectrometer Study of charged particles and nuclei with rigidity 0.5 GV– few TV Direct search for antimatter (antihelium) Indirect search for Dark Matter On International Space Station from October 2006

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+ -

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Cosmic ray sensitivity for dark matter search Cosmic-ray spectroscopy with high precision in particle identification: p+ Rejection > 106 e+ Efficiency > 90%

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AMS02 on International SpaceStation High Statistics (10 10 ev) + Good Discrimination Space: Thermal Environment (day/night: T~100oC) Vibration (6.8 G RMS) and G-Forces (17G) Limitation : Weight (14 809 lb) and Power (2000 W) Vacuum: < 10-10 Torr Reliable for more than 3 years – Redundancy Radiation: Ionizing Flux ~1000 cm-2s-1 Orbital Debris and Micrometeorites Must operate without services and human Intervention

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Superconducting Magnet Analyzing power BL2 = 0.8 Tm2 B.Blau Talk 12 OG.1.5

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Flux Return Coils Dipole Coils He Vessel B B 2500 Liters Superfluid He Superconducting Magnet

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S.Gentile Talk 14 OG.1.5, 1-P-109 : 3 –300GeV e+/p rejection 102 –103 in 1.5 – 300 GeV with ECAL e+/p rejection >106

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TRD Support Structure Modules Honeycomb Support Panels Mechanical Accuracy <100mm 328 chambers = 5248 tubes

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TOF Layers Trigger Time-of-flight (velocity). Up/Down Separation |Charge| Determination (dE/dx) 120 ps Time Resolution TOF system Time-of-flight system 8 m2 Total Area 4 Planes (2 upper,2 lower)

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Dual Photomultipliers for Redundancy and time resolution Scintillator Paddles D.Casadei 1-P-110 Scintillator Paddles With Phototubes at Both Ends

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Silicon Tracker Rigidity (DR/R  2% for 1 GeV Protons) with Magnet Signed Charge (dE/dx) 8 Planes, ~6m2 Pitch (Bending): 110 mm (coord. res. 10 mm ) Pitch (Non-Bending): 208mm (coord. res. 30 mm ) E. Cortina Talk 2 HE 3.4, 2-P-297

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Silicon Tracker Ladder

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Aerogel Radiator Mirror Cerenkov Cone Photomultipliers Ring Imaging Cerenkov Counter Accurate Velocity Measurements via Opening Angle of Cerenkov Cone  Isotopic Separation. |Q| measurements D/ ~ 0.1% Cosmic Ray Propagation. Additional Particle Identification capability M.Buenerd Talk 13 OG.1.5

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3D sampling calorimeter 9 superlayers of 10 fiber/lead planes each alternate in x and y scintillating fibers viewed by PMT 16.4 X0 radiation length Measure energy and (angle) of g, e+,e- Distinguish e, p better than 103 in the range 1 GeV-1 TeV. Electromagnetic Calorimeter

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Electromagnetic Calorimeter 10-3 p Rejection at 95% e Efficiency Via Shower Profile p e

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ECAL Prototype After Testbeam Al Support Structure PMT’s + Readout PMT + Readout Housing

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Energy resolution /E= (9.84 ± 0.13)/E  (1.95 ± 0.02) %

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E.Cortina Talk 15 OG.1.5

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A on board backup is forseen once a month by austronauts AMS Computer facility

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Max Power 2000W

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Star Tracker Angular resolution 30 arcsec

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|Q| measured from Tracker, RICH, TOF.  Q measured from tracker. Velocity b measured from TOF, TRD, RICH. Hadron Rejection TRD, ECAL. Main design characteristics: Minimum Xo (up to ECAL) Many independent measurement of b Acceptance 0.5 m2 anti-He search Hadron/positron Db/b = 0.1 % to distinguish 9Be,10Be, 3He,4He isotopes. Rigidity R= pc/|Z| e GV resolution 20% at 0.5 TV and Helium resolution of 20% at 1TV.

Conclusions: 

Conclusions AMS02 will measure charged cosmic rays up to few TeV rigidity for 3 to 5 year on International Space station from October 2006. To search for: Antimatter Dark Matter Cosmic Ray Fluxes and propagation Search for isotopes High Energy g Many channels are measured simultaneously, which will give a strong constrain on models and increase the potential of discovery.