1. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe1 The AMS experiment

2. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe2

3. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe3 The purpose of the AMS experiment is to perform accurate, high statistics, long duration measurements in space of energetic (0.1 GV - few TV) charged CR including particle identification - energetic gamma rays. Nobel Prizes, (1)Pulsar, (2)Microwave, (3)Microwave (4)Binary Pulsars, (5)Solar neutrino X Ray sources

4. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe4 International commitments to AMS USA A&M FLORIDA UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER UNIV. OF MARYLAND-DEPRT OF PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE UNIV. - NEW HAVEN MEXICO UNAM DENMARK UNIV. OF AARHUS FINLAND HELSINKI UNIV. UNIV. OF TURKU FRANCE GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE GERMANY RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE ITALY ASI CARSO TRIESTE IROE FLORENCE INFN & UNIV. OF BOLOGNA INFN & UNIV. OF MILANO INFN & UNIV. OF PERUGIA INFN & UNIV. OF PISA INFN & UNIV. OF ROMA INFN & UNIV. OF SIENA NETHERLANDS ESA-ESTEC NIKHEF NLR ROMANIA ISS UNIV. OF BUCHAREST RUSSIA I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. SPAIN CIEMAT - MADRID I.A.C. CANARIAS. SWITZERLAND ETH-ZURICH UNIV. OF GENEVA CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) KOREA EWHA KYUNGPOOK NAT.UNIV. Y96673-05_1Commitment PORTUGAL LAB. OF INSTRUM. LISBON ACAD. SINICA (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) TAIWAN

5. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe5 Particle identification = the name of the game For every antiproton at some energy there are 10,000-100,000 protons For every positron at some energy there are ~10,000 protons which have same charge sign Secondary particles (long and short lived) are locally produced Single scatters change apparent particle charge sign in simple trackers

6. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe6 G.F. 5000 cm 2 sr Exposure > 3 yrs dP/P 2 ~ 0.004  2.5 TV, h/e = 10 -6 (ECAL +TRD); Δx=10µm; Δt=100ps 3x3x3m, 7 t

7. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe7 Contraints for a Space Experiment –Thermal Environment (day/night:  T~100 o C) –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 -2 s -1 –Orbital Debris and Micrometeorites –Must operate without services and human Intervention – Superconducting Magnet

8. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe8 Alpha Magnetic Spectrometer - AMS-01 First flight, STS-91, 2 June 1998 (10 days) TOF Tracker Magnet TOF Cerenkov Counter AMS

9. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe9 Flux Return Coils Dipole Coils He Vessel B B 2500 Liters superfluid He Superconducting Magnet Analyzing power BL 2 = 0.8 Tm 2

10. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe10 The coils completed

11. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe11 Now inside the cryostat

12. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe12 : 3 –300GeV e+/p rejection 10 2 –10 3 in 1.5 – 300 GeV with ECAL e+/p rejection >10 6 TRD detector to separate e + from protons

13. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe13 TRD detector 20 layers,328 chambers,5248 tubes Mechanical accuracy <100μm Assembly ready CERN beamtest with TRD prototype: proton rejection > 100 up to 250 GeV at electron efficiency 90% reached Single tube spectra for p+/e separation.

14. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe14 Silicon Tracker Rigidity (  R/R  2% for 1 GeV Protons) with Magnet Signed Charge (dE/dx) 8 Planes, ~6m 2 Pitch (Bending): 110  m (coord. res. 10  m ) Pitch (Non-Bending): 208  m (coord. res. 30  m ) Charge measurent up Z ~ 26

15. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe15 Aerogel Radiator(n=1.03, 3cm) NaF radiator (n=1.33, 0.5cm) Mirror Cerenkov Cone Photomultipliers Ring Imaging Cerenkov Counter Accurate Velocity  /  = (0.67  0.01)*10-3% (test beam) Isotopic Separation. |Q| measurements up Z~ 30 8.5 x 8.5 mm 2 spatial pixel granularity

16. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe16 due to limitations in weight, space experiments have an ECAL section, normally with limited thickness Standard measurement for “thickness” is the radiation length (X 0 ) which is related to the development of the energy deposition –a detector with high X 0 has a good energy and angular resolution and it is capable of measuring particles in the energy range 10GeV-1TeV with good accuracy (<5%) –AGILE : 1.5X 0 –GLAST 10X 0 –AMS-02 : 16.1 X 0 Calorimetry in space AMS: 3D sampling calorimeter: measure energy (few % resolution) and angle (1° - 0.5° angular resolution) 10 -3 p  rejection at 95% e  efficiency via shower profile 1 GeV - 1 TeV

17. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe17 Lead foil (1mm) Fibers (  1mm) y x z particle direction 1.73mm p p ee FIBER LEAD Sampling calorimeter with lead foils and scintillating fibers Basic block is superlayer: 11 lead and 10 fiber layers 9 superlayers with alternating x and y readout Total thickness is 166mm, corresponding to 16.2 X 0 Total weight 634 kg Electromagnetic calorimeter

18. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe18 2007 2008 Thermal vacuum test at ESA, Holland 2007 Assembly at CERN Final integration in 2007 at CERN Final testing in ESA vacuum chamber (NL)

19. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe19 Charge measurements B Ne P Ca Fe ToF, Tracker, RICH performance verified at heavy ion test beam (CERN,GSI)

20. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe20 He C N Charge measurement: TOF, Tracker and RICH Verified by heavy ion beam tests at CERN & GSI. TOF LiHe Be C O N Si Test Results from Tracker detector Nuclei separation

21. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe21 6 months 1 day 1 year 10 Be (t 1/2 =1.5Myr) / 9 Be will allow to estimate the propagation time and size of the ISM B is secondary produced in nuclear interaction, C is primary produced in stars. B/C is sensitive to the diffusion constant 3 He/ 4 He ratio is sensitive to the density of the ISM AMS-02 capabilities Beryllium Boron Helium 6 months 1 year 1 day

22. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe22 One propagation model of our Galaxy

23. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe23 it is shown that Galactic cosmic rays can be effectively confined through magnetic reflection by molecular clouds, Another propagation model including static magnetic fields and gas clouds Integral excess of positrons in bulge because positrons are trapped in magnetic mirrors between gas clouds

24. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe24 Magnetic fields observed in spiral galaxies A few uG perpendicular to disc: Strong convection  to disc? A few µG in the disc: can lead to slow radial diffusion Isotropic diffusion assumes randomly oriented magnetic turbulences. Preferred magnetic field directions -> anisotropic diffusion disk fieldline

25. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe25 Antiprotons B/C ratio Preliminary results from GALPROP with isotropic and anisotropic propagation Summary: with anisotropic propagation you can send charged particles whereever you want and still be consistent with B/C and 10 Be/ 9 Be

26. May, 18. 2007 PPC07, College Station, W. de Boer, Univ. Karlsruhe26  AMS is a High Energy Physics detector in space foreseen to operate on the ISS for 3 years  Asked by NASA to be Ready For Flight end 2008  The cosmic rays, including gamma rays, will be measured with a high accuracy from the GeV to the TeV range  Unique opportunity to study properties of our Galaxy and its dark matter, including how particles propagate Summary