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AMS-02 Experiment (Alpha Magnetic Espectrometer)

AMS-02 Experiment (Alpha Magnetic Espectrometer). Detector and Expectations. Diago UniverseNet School ‘09 IAC (Spain) October 2, 2009. AMS-01. AMS-01 was launched on the Shuttle Discovery on 2th June 1998. 180 hours of data: 10 8 events.

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AMS-02 Experiment (Alpha Magnetic Espectrometer)

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  1. AMS-02 Experiment(Alpha Magnetic Espectrometer) Detector and Expectations • Diago UniverseNet School ‘09 • IAC (Spain) October 2, 2009

  2. AMS-01 • AMS-01 was launched on the Shuttle Discovery on 2th June 1998. • 180 hours of data: 108 events. Discovery with AMS-01 seen from MIR

  3. AMS-02 AMS-01: Results • Feasible proyect • Measures of fluxes p, He3, He4, e+, antiprotons. • Secondary spectrums near earth orbit under the geomagnetic cutoff: • Protons • Leptons • Helium • New limits to the existence of antihelium AntiHe/He<1.1x10-6 AntiHe/He<0.9x10-4 (Buffington)

  4. Detector’s Features AMS-02 • Second part of the AMS Experiment. • Developed with international cooperation. • It will be on ISS in autumn 2010. • General points: active 3 years at minimum + acceptance of 0.5 m2.sr 1010 nuclei

  5. Detector’s Features Size: 3m x 3m x 3m Weight: 7 tons Subdetectors: TRD TOF TRACKER Anticounter RICH ECAL

  6. Studies ready to be done • Cosmic rays composition (TRD, TRACKER, RICH) • Photon detection up to 1 TeV (TRACKER, ECAL) • Propagation (TRACKER, RICH) He3/He4 B/C Be10/Be9 • Antimatter searching Z>1 (TRACKER, RICH) • Dark matter searching (TRD, TRACKER, RICH) Size: 3m x 3m x 3m Weight: 7 tons

  7. How does it work?

  8. Transition Radiation e/p separation e- Discrimination e/p

  9. e- Transition Radiation e/p separation p

  10. Transition Radiation e/p separation e- Discrimination e/p e/p~102-103 x 20 AMS Collaboration

  11. Time of Flight LV1, dir, β, Z LV1: Trigger

  12. Time of Flight LV1, dir, β, Z LV1: Trigger selection

  13. Time of Flight LV1, dir, β, Z LV1: Trigger selection ttravel= 1 ns 130 ps precision downwards-upwards

  14. Time of Flight LV1, dir, β, Z e-

  15. Time of Flight LV1, dir, β, Z e- e-

  16. Time of Flight LV1, dir, β, Z e- e- e+

  17. Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p

  18. Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p Charge Z separation (up to 1 GeV)

  19. Time of Flight LV1, dir, β, Z AMS Collaboration

  20. Time of Flight LV1, dir, β, Z LV1: Trigger selection Dir: downwards-upwards e-/antiP e+/p Charge Z separation Mesure of b with few % precision

  21. Superconducting Magnet AMS-01 Nd-Fe-B BL2= 0.14 T·m2 AMS-02 Superconducting BL2=0.86 T·m2 R=2.5 TV

  22. Silicon Tracker Z,R Measure of rigidity Measure of charge

  23. Silicon Tracker Z,R AMS Collaboration Combined Z measurements for 4 or more ladders on the K and S sides

  24. Anticounter Acceptance

  25. RICH β, Z n(NaF)=1,335 n(aerogel)=1,05

  26. RICH β, Z AMS Collaboration Charge Z Speed b AMS Collaboration

  27. Electromagnetic calorimeter e/p separación, E Discrimination e/p Measure of energy AMS Collaboration

  28. What is the information that we get?

  29. Separation e/p Speed  Charge Z Rigidity R Energy E Direction dir Mass m

  30. Separation e/p: 106 Speed  Charge Z Rigidity R Energy E Direction dir Mass m

  31. Separation e/p Speed : s(b)/b=10-3 Charge Z Rigidity R Energy E Direction dir Mass m

  32. Separation e/p Speed  Charge Z:s(Z)/Z=0.2 Rigidity R Energy E Direction dir Mass m

  33. Separation e/p Speed  Charge Z Rigidity R: 2.5 TV Energy E Direction dir Mass m

  34. Separation e/p Speed  Charge Z Rigidity R Energy E: Direction dir Mass m

  35. Separation e/p Speed  Charge Z Rigidity R Energy E Direction dir: Distinction power: 10-9 Mass m

  36. Separation e/p Speed  Charge Z Rigidity R Energy E Direction dir Mass m: 2%(<1GeV)

  37. What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma

  38. What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles

  39. Composition: Fluxes C (10 days) e- (3 years) Fe (1 year) He (1 month) P (1 week) PAMELA PAMELA PAMELA AMS Collaboration

  40. PAMELA PAMELA Composition: Fluxes AMS Collaboration PAMELA Collaboration

  41. What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles • Ratios

  42. Composition: ratios (1 day) Interestelar medium density Diffusion parameter AMS Collaboration

  43. What can be done with all this information? • What kind of particle is it? • Lepton, hadron, gamma • Flux of the different particles • Ratios • Isotopic separation

  44. Compostion: isotopic separation He3 He4 Be9 Be10 p D Rui Pereira, 2006 AMS Collaboration

  45. What can be done with all this information? Is AMS-02 better than PAMELA? Of course!

  46. AMS-01 (expected) PAMELA What can be done with all this information? AntiHe/He

  47. What can be done with all this information? Is AMS-02 better than FERMI? We will try it with photons

  48. AMS-02: Models constrains An anomalous positron abundance in cosmic rays with energies 1.5-100 GeV. O. Adriani etal 2009 Why this anomaly?

  49. MDM=10 TeV DM+DM W+W- sannv=6·10-22 cm3/sec M. Cirelli, A. Strumia 0903.3381v2 e-+e+ antip/p AMS-02 e+/(e++e-) e-+e+ Posible answers: Dark matter contribution?

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