1 / 36

The Alpha Magnetic Spectrometer (AMS) on the International Space Station (ISS)

The Alpha Magnetic Spectrometer (AMS) on the International Space Station (ISS). Maria Ionica I.N.F.N. Perugia Maria.Ionica@pg.infn.it International School of Cosmic-Ray Astrophysics 13 th Course: Relativistic Astrophysics and Cosmology 2-14 June, 2002, Erice. Outline.

ahmed-lott
Download Presentation

The Alpha Magnetic Spectrometer (AMS) on the International Space Station (ISS)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript


  1. The Alpha Magnetic Spectrometer (AMS) on the International Space Station (ISS) Maria Ionica I.N.F.N. Perugia Maria.Ionica@pg.infn.it International School of Cosmic-Ray Astrophysics 13th Course: Relativistic Astrophysics and Cosmology 2-14 June, 2002, Erice

  2. Outline • Physics objectives of the AMS experiment • AMS-01 on the space Shuttle Discovery in 1998 • Results obtained with AMS-01 from the STS-91 flight • The Silicon Tracker for the AMS-02 experiment on the ISS

  3. AMS - a particle physics experiment in space • Existence of the matter-antimatter asymmetry in our region of the Universe • This asymmetry could be explained assuming one of the following scenarios: • The asymmetry is assumed as an initial condition • The Universe can be globally symmetric, but locally asymmetric • A dynamic mechanism which caused the asymmetry, starting from an initial symmetric phase (CP violation, GUT) • due to the limited energy which can be reached at accelerators, these problems can only be studied by performing very accurate measurement of the composition of CR • The AMS experiment is using the Universe as the ultimate laboratory.

  4. AMS physics goals • To search for Nuclear Antimatter (antiHe,antiC) in space with a 10-9 sensitivity (103 -104 better than current limits). • To search for supersymmetric Dark Matter by high statistics, precision measurements of e,  and p- spectrum. • To study Astrophysics: • High statistics, precision measurements of D, 3He, 4He, B, C, 9Be, 10Be spectrum • B/C: to understand CR propagation in the Galaxy (parameters of galactic wind). • 10Be/9Be: to determine CR confinement time in the Galaxy.

  5. Anti-nuclei in cosmic radiation • Researches for evidence of antimatter in CR have been carried out before AMS only by stratospheric balloons • If the antimatter exists it could be at the level of the clusters of galaxies • Anti-protons and positrons are not good indicators for existence of nuclear antimatter: they can be produced by the interaction of the primary cosmic rays with the interstellar medium; • The probability to have an antinucleus produced in primary interactions is less less than 10-10 for anti3He and less than 10-56 for antiC: “discovery of only one nucleus of antiC, would be the proof of the existence of antimatter in Universe”. (Steigman.G, Ann. Rev. Astron. Astrophys. 14 (1976)339)

  6. AMS-01 on Discovery during STS-91 Flight

  7. AMS01 detector • Magnet: Nd2Fe14B, BL2= 0.15 TM2 • T.o.F: Four planes of scintillators; •  and Z measurements, up/down separation • Tracker: Six planes of ds silicon detectors; • Charge sign, dE/dX up to Z=8, Rigidity (p/Z) • Anticounters: • Veto stray trajectories and bckgnd particles from magnet walls • Aerogel Threshold Čerenkov: •  measurements (13 GeV/c) for better e/p separation • Low Energy Particle Shielding (LEPS): • Carbon fibre, shield from low energy (<5MeV) particles

  8. AMS deintegration at CERN: Silicon Tracker on assembly jig

  9. AMS Silicon Detectors on the Automatic testing facilty (Perugia)

  10. AMS silicon tracker module

  11. AMS silicon tracker module

  12. AMS Silicon Tracker plane equipped with Silicon Ladders (STS-91)

  13. AMS-01- STS-91 Flight Results It was a successful flight !! • Detector test in actual space conditions • Good performance of all subsystems • Physics results: • Antimatter search • Charged cosmic ray spectra (p,e,D,He,C,N,O) • Geomagnetic effects on cosmic ray

  14. New limit on antiHe

  15. Event reconstruction Measure Rigidity (R, R1, R2) Sign of Rigidity Absolute value of Z Velocity (b) Apply cuts Test antiHe hypothesis Compute limit

  16. AMS-01 STS-91 Flight Physics Results (1)

  17. RESULTS on Primary Cosmic Ray Spectra

  18. Electron data

  19. Energy Range of AMS on ISS p+ up to several TeV p- up to 200 GeV e- up to O(TeV) e+ up to 200 GeV He,….C up to several TeV anti – He…C up to O(TeV) g up to 100 GeV Light Isotopes up to 20 GeV

  20. AMS-02 Tracker (1) • Coordinated by INFN Perugia in collaboration with University of Geneva, University of Aachen, University of Turku and NLR. • Aim: • Rigidity (P/Ze) measurements • Sign of Charge • Absolute Charge (dE/dX , in addition to ToF system) • Tracker detector based on 8 thin layers of double-sided silicon microstrips, with a spatial resolution better than 10 mm,  200.000 electronics channel and  800 W of power. • This complex detector, qualified for operation in space, with about  6 m2 of active surface will be the largest ever built before the LHC @ CERN.

  21. AMS-02 Tracker (2) • Operating Temperature: -10/+25 °C • Power Dissipation inside the magnet: 1 W/ladder, in total 192 ladders • dP/P =  2 % @ 1 GeV ( 8% in AMS-01) (for protons) • The planes alignment will be monitored by a IR laser alignment system (as in case of AMS-01).

  22. AMS-02 Tracker (3)(from AMS-01)

  23. Sensitivity of future CR experiments

  24. Conclusions • AMS-01 has successfully been tested during STS-91 flight providing important information on operating in actual space conditions • AMS-01 data allows to study the primary and trapped CR fluxes in the energy range from 100 MeV to about 100 GeV • AMS-02 will extend the accurate measurements of CR spectra to unexplored TeV region opening a new window for the search for Antimatter and Darkmatter.

  25. AMS-02 on ISS

More Related