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Cosmic-Rays Astrophysics with AMS-02

Cosmic-Rays Astrophysics with AMS-02. Alberto Oliva* on the behalf of the AMS Collaboration *University and INFN Perugia, Italy. Outline High Energy Astrophysics with AMS The AMS-02 Detector, and the Measurement Methods Expected Physics. AMS-02 experiment.

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Cosmic-Rays Astrophysics with AMS-02

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  1. Cosmic-Rays Astrophysics with AMS-02 Alberto Oliva* on the behalf of the AMS Collaboration *University and INFN Perugia, Italy Outline • High Energy Astrophysics with AMS • The AMS-02 Detector, and the Measurement Methods • Expected Physics

  2. AMS-02 experiment High Energy Particle Physics in Space (ISS): • Large Acceptance, Long Duration  High Statistics • Charged Particles & Nuclei Spectra • High Energy Gamma Rays Physics goals: • Search for Primordial Antimatter by Direct Detection of Antinuclei (He/He<10-9) • Dark Matter Signatures in p, e+, d,  spectra • Production, Acceleration and Propagation of Cosmic-Rays • Solar Modulation

  3. AMS-02 experiment High Energy Particle Physics in Space (ISS): • Large Acceptance, Long Duration  High Statistics • Charged Particles & Nuclei Spectra • High Energy Gamma Rays Physics goals: • Search for Primordial Antimatter by Direct Detection of Antinuclei (He/He<10-9) • Dark Matter Signatures in p, e+, d,  spectra • Production, Acceleration and Propagation of Cosmic-Rays • Solar Modulation

  4. CR spectrum and AMS-02 expectation H »1010 H »109 He »107 C, O »106 Be, Fe He C O Fe Be

  5. Cosmic Nuclei Astrophysics Secondaries > 105 y Source Our Galaxy SNR Shock Wave Primaries »107 y AMS-02

  6. Cosmic Nuclei Astrophysics > 105 y Source Our Galaxy SNR Shock Wave Cosmic rays abundances »107 y AMS-02

  7. Cosmic Nuclei Astrophysics > 105 y Source Our Galaxy SNR Shock Wave Charge/Mass Distinction »107 y AMS-02

  8. Cosmic Nuclei Astrophysics > 105 y Source Our Galaxy SNR Shock Wave Maurin, Taillet, FD A&A 2002 sub-Fe/Fe B/C AMS-02 Charge Distinction

  9. Cosmic Nuclei Astrophysics > 105 y Mass Distinction Source Our Galaxy SNR Shock Wave 6Li/7Li 3He/4He Maurin, Taillet, FD A&A 2002 AMS-02 Charge Distinction

  10. Cosmic Nuclei Astrophysics HALO > 105 y Source Our Galaxy T(10Be) » 1.5£106 y SNR Shock Wave »107 y AMS-02 10Be/9Be

  11. AMS-02 Detector • Cryogenic Superconducting Magnet of 0.8 T • TOF: 4 layers of scintillators (150 ps resolution) • Tracker: 8 layers of Si detectors (10 (30) m) • RICH Detector (/ » 0.1/Z %) • TRD Detector: p/e rejection in 103 • Pb/Sc EM Calorimeter: p/e rejection 104 • Geometric acceptance of 0.45 m2¢sr • Z measurement up to Iron • A global statistics above 1010 particles • Detector redundancy (charge, velocity) • Trigger: TOF, ACC (no ACC for ions) or ECAL for 

  12. Charge measurement • The charge evaluation is redundant • Tracker, TOF: energy deposition by ionization • RICH: number of photons in the Cherenkov ring B Beam test C Fe Be N O Ne F

  13. Rigidity measurement • The AMS-02 Si Tracker: • Silicon double-sided sensors • 8 layers arranged in 5 planes • Resolution < 10 m in the bending direction • A rigidity determination of 2% at 10 GV Beam test <>» 5 m Simulation

  14. Velocity measurement RICH • Redundant measurements • TOF:  = L/t with /» 1% • RICH: with /» 0.01% Beam test Beam test

  15. Mass measurement • The AMS-02 spectrometry • Tracker for rigidity and charge • RICH for velocity and charge • Isotopic distinction up to » 10 GeVn 10Be/9Be Simulation

  16. Mass measurement • The AMS-02 spectrometry • Tracker for rigidity and charge • RICH for velocity and charge • Isotopic distinction up to » 10 GeVn • Two radiators: • NaF (n = 1.334) • Aerogel (n = 1.050) 10Be/9Be Simulation

  17. Long term measurement • After 3 years of “full“ magnetic spectrometry: • Lowering TRD gain by a factor 20 • Measure  for charges up to Iron • 10 – 30 % energy resolution • From 200 to 4000 GeV/n from the TRACER collaboration

  18. Expected 1 day 1 week d/p 3He/4He »107 particles »106 particles 6 months 1 year B/C 10Be/9Be »107 particles »107 particles

  19. Conclusions • AMS-02 in the integration phase and will be installed on the ISS in 2009 • AMS-02 will perform high statistic measurement of all chemical species up to Iron in CR in a wide energy spectrum • AMS-02 will play a key role in the CR Astrophysics studies THANK YOU

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