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AMS

The Alpha Magnetic Spectrometer Experiment (AMS). AMS. Guoming Chen IHEP Beijing . AMS: A TeV (10 12 eV) Magnetic Spectrometer in Space 3m x 3m x 3m, 7t, ~ 0.5m 2 sr. +y03K193_2ea. AMS is an international collaboration of 16 countries, 60 institutes and 500 physicists. . FINLAND.

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AMS

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  1. The Alpha Magnetic Spectrometer Experiment (AMS) AMS Guoming Chen IHEP Beijing

  2. AMS: A TeV (1012 eV) Magnetic Spectrometer in Space 3m x 3m x 3m, 7t, ~ 0.5m2 sr +y03K193_2ea

  3. AMS is an international collaboration of 16 countries, 60 institutes and 500 physicists. FINLAND RUSSIA HELSINKI UNIV. UNIV. OF TURKU I.K.I. ITEP KURCHATOV INST. MOSCOW STATE UNIV. DENMARK UNIV. OF AARHUS NETHERLANDS GERMANY ESA-ESTEC NIKHEF NLR RWTH-I RWTH-III MAX-PLANK INST. UNIV. OF KARLSRUHE KOREA USA EWHA KYUNGPOOK NAT.UNIV. FLORIDA A&M UNIV. JOHNS HOPKINS UNIV. MIT - CAMBRIDGE NASA GODDARD SPACE FLIGHT CENTER NASA JOHNSON SPACE CENTER TEXAS A&M UNIVERSITY UNIV. OF MARYLAND-DEPRT OF PHYSICS UNIV. OF MARYLAND-E.W.S. S.CENTER YALE UNIV. - NEW HAVEN FRANCE ROMANIA CHINA BISEE (Beijing) IEE (Beijing) IHEP (Beijing) SJTU (Shanghai) SEU (Nanjing) SYSU (Guangzhou) SDU (Jinan) GAM MONTPELLIER LAPP ANNECY LPSC GRENOBLE ISS UNIV. OF BUCHAREST SWITZERLAND ETH-ZURICH UNIV. OF GENEVA SPAIN CIEMAT - MADRID I.A.C. CANARIAS. ACAD. SINICA (Taiwan) AIDC (Taiwan) CSIST (Taiwan) NCU (Chung Li) NCKU (Tainan) NCTU (Hsinchu) NSPO (Hsinchu) 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 MEXICO UNAM PORTUGAL LAB. OF INSTRUM. LISBON 95% of the $1.5B to build AMS has come from our international partners based on NASA’s commitment to deploy AMS on the ISS.

  4. First flight AMS-01 Approval: April 1995, Assembly: December 1997, Flight: 10 days in June 1998 AMS y96207_05b

  5. Unexpected results from first flight: 1- the existence of two Spectra in proton flux 1.0<M<1.1 0.8<M<0.9 Expected Spectra due to Earth’s magnetic field Flux (m2 sec sr MeV)-1 0.6<M<0.7 0.4<M<0.5 M<0.3 Phys. Lett. B472 (26 Jan 2000) 215-226

  6. Unexpected results from first flight: 2- There are many more positrons (e+) than electrons (e-) SecondSpectra Geomagnetic latitude (radians) Phys. Lett. B484 (27 Jun 2000) 10-22

  7. Unexpected results from first flight: 80 100 3.650±0.09 He4 Energy/2 10 60 1 Events 40 -0.8 -0.4 0 0.4 0.8 40 20 30 20 Events 0 10 10 5 (GeV) 0 1 2 3 4 5 6 3- He4 and He3 isotopes are completely separated in space M ΘM Mass (GeV) Phys. Lett. B494 (2000) 193-202 These results were not predicted by any cosmic ray model

  8. Construction of the AMS-02 Superconducting magnet Racetrack Coils (2x6) Dipole Coils (2x) 0.86 T 2,500 lSuperfluid HeDuration: 3-5 years

  9. Transition Radiation Detector: TRD Identify e+, reject P works for 20y 20 layers

  10. BEAM TEST at CERN Design rejection 5248 tubes

  11. Time of Flight (TOF) AMS TRD TOF Super- conducting Magnet Cryocooler He Vessel Coils Tracker TOF RICH ECAL Measures the time of particles to ~ 100 picoseconds Charge measurement up to Z=26 with de/dx

  12. TRD (5248 channels) TOF Tracker (200000 channels) Superconducting Magnet 2500 L SF Helium TOF RICH (10880 channels) ECAL (1300 ch. Silicon Tracker, 8 planes

  13. Test results from CERN identify all nuclei simultaneously S side 200 000 channels alignment 3m K side

  14. Precise measurement of the velocity & charge Particle Charge Z Velocity  CerenkovRadiator Conical Reflector Photo- detectors AMS Ring Imaging CHerenkov (RICH) 10,880 photodetectors

  15. Δv/v = 0.001 (1-)/1000 Li C He Ca O RICH test beam E=158 GeV/n charge measurement up to 30 Z (1-v/c)/1000 Single Event Displays

  16. ECAL: A measurement of the direction & energy of gamma rays and electrons TRD (5248 channels) TOF Superconducting Magnet Tracker (200000 channels) 2500 L SFHelium TOF RICH (10880 channels) e, γ ECAL (1300 ch. p Completed Flight Module Cut-away view of fibers and lead

  17. ECAL capability Complementary with TRD, ECAL can reject hadron by a factor of 200 at high energy

  18. Accelerator testing of AMS and components Tandem heavy ion Van de Graff, Catania High intensity proton cyclotron, Indiana Heavy ion accelerator, Darmstadt High energy proton and ion accelerator, Geneva

  19. Results from accelerator tests “Hubble telescope” for charged particle He Simultaneous measurement of all nuclei Li C B O N Mg Ne F Na Si Be Al S P Number of Events Cl Ar Ca K Sc Ti V Cr Mn Fe Co Atomic Number Δv/v = 0.001 103 Δ t = 100 ps Δx = 10 µm 2500 102 1500 Events Events/20 ps 10 500 -1 2 0 1 -2 Time of Flight (ns) (1-)/1000 1 Events y04K513_05

  20. Cosmic test early 2008, every piece works well

  21. AMS02 Cosmic Test

  22. Space qualification Testing in 2008 LARGE SPACE SIMULATOR AT ESA The detector is on schedule to be sent to KSC in early 2009

  23. Search for Antimatter in the Universe AMS AMS in Space Search for the origin of the Universe Search for the existence of anti Universe Accelerators The Big Bang origin of the Universe requires matter and antimatter to be equally abundant at the very hot beginning

  24. AMS-01 Experimental work on Antimatter in the Universe Direct search Baryogenesisconditions Search fornew CP BELLE BaBarFNAL KTeV CERN NA-48 CDF, D0 Search forProton decay LVD, ICARUS,Super K, … Major worldwide efforts with negative results Results negative LHC-bATLAS CMS AMS-02Increase in sensitivity: x 103 – 106Increase in energy to ~TeV y06K299a

  25. AMS-02 Antihelium Limits Current antimatter searches are limited He/He (CL 95%) y06K301

  26. 2x109 nuclei If no antimatter is found => there is no antimatter within ~ 1000 Mpc. Other possible solutions: The existence of a new source of CP Violation The existence of Baryon, Lepton Number Violation Grand Unified Theory Electroweak Theory SUSY These are central research topics for the current and next generation of accelerators world wide the Foundations of Modern Physics

  27. Indirect dark matter search • Space  avoid contamination from atmospheric secondaries • Multichannel analysis

  28. Dark Matter Search Through Positron Assume HEAT excess come from χ

  29. 10 -3 Spectra with Dark Matter 10 -4 Normal spectra for anti-proton/proton 10 -5 1 10 100 Kinetic Energy (GeV) A leading theoretical candidate for Dark Matter A supersymmetric particle with Mχ = 840 GeV. P/P

  30. Dark Matter Search Through Antiproton

  31. T.Prodanovi´c et al., astro-ph/0603618 v1 22 Mar 2006 Space Experiments Ground Experiments EGRET upper limits AMS-02 Dark matter search through high energy diffuse gammas g e− e+ P− P+ E− E+ Unique constraints P+ = E+ = P− = E− The diffuse gamma-ray spectrum of the Galactic plane 40o < 1 < 100o, |b| < 5o • Pointing precision of 2 arcsec • UTC time (from GPS, μsec accuracy) allows to relate AMS measurements with other missions

  32. 104 101 H He  (s-1 m-2 sr-1 GeV-1) 10-2 B Li Be C N O 10-5 Ne F Mg 10-8 Na Si Al S P K Ar 10-11 Cl Ca Sc Ti Mn V Cr Fe Co Ni 0.1 1 10 Ekin/n (GeV) 100 1000 Precision study of the properties of Cosmic Rays Composition at different energies (1 GeV, 100 GeV, 1 TeV) Charge measurement up to 30 1 5 10 Z 15 20 25 Isotope measurement: D/P, He(3)/He(4), Be(9)/Be(10)…

  33. Proton Flux up to 2 TeV

  34. Helium Flux up to 1TeV/Nuc

  35. Electron Flux up to 1TeV

  36. 3He/4He Ratio Measurement

  37. B/C measurement relative fluxes regardless of the magnetic field AMS will measure the ratio B/C up to and collect after 3 years 105 C with E > 100 GeV/A 104 B with E > 100 GeV/A

  38. 10Be / 9Be Measurement C.Mana • the cosmic ray • confinement • time in the galaxy, • ii) the mean density of • interstellar material • traversed by cosmic rays. One of the most important measurements in cosmic ray physics y01K22ge.ppt

  39. Background determination for dark matter search The precise measurement of all the nuclei and their isotopes will provide stringent constraint on cosmic propagation models, which will in turn give precise background prediction for positron, anti-proton and gamma rays

  40. Conclusion • AMS02 has been built and tested, ready to be launched • Search for anti-Helium at the sensitivity of 10-9, will exclude anti-matter within Billion pc • Search for dark matter through positron, antiproton and gamma spectrum • Precise measurement of nuclei and their isotopes up to z=30 will provide precise prediction of background for dark matter search • Global fitting of the positron, anti-proton and gamma rays worldwide may give a hint to the solution of dark matter

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