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The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia TAUP 2001 Laboratori Nazionali del Gran Sasso, Italy.

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Presentation on theme: "The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia TAUP 2001 Laboratori Nazionali del Gran Sasso, Italy."— Presentation transcript:

1 The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia TAUP 2001 Laboratori Nazionali del Gran Sasso, Italy September 8-12, 2001

2 B. Alpat, INFN Sezione di Perugia The AMS Physics To search for Antimatter (He,C) in space with a sensitivity of 10 2 to 10 3 better than current limits. To search for dark matter  High statistics precision measurements of e ,  and p spectrum. To study Astrophysics.  High statistics precision measurements of D, 3 He, 4 He, B, C, 9 Be, 10 Be spectrum  B/C: to understand CR propagation in the Galaxy (parameters of galactic wind).  10 Be/ 9 Be: to determine CR confinement time in the Galaxy.

3 B. Alpat, INFN Sezione di Perugia AMS-01 Configuration on STS-91 Flight STS-91 Flight, June 2-12 th, 1998 Magnet: Nd 2 Fe 14 B, BL 2 = 0.15 TM 2 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 (up to 3 GeV/c) for better e/p separation Low Energy Particle Shielding (LEPS): Carbon fibre, shield from low energy (<5MeV) particles

4 B. Alpat, INFN Sezione di Perugia AMS-01: STS-91 Flight  30 hours before and  105 hours after rendezvous with MIR (total of  135 hours including  11 hours of albedo measurements) Shuttle altitude ranged from 320 to 390 km Latitudes  51.7°, All longitudes (except S.A.A.) A total of 100 million events recorded with event rates ranging from 100 Hz to 700 Hz (corresponding to 95%  40% DAQ livetime)

5 B. Alpat, INFN Sezione di Perugia 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)  Geomagnetic effects on cosmic ray

6 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Search for Antihelium- Contamination of Z=1 in the Z=2 sample: <10 -4 tracker only <10 -7 tracker+TOF Rigidity resolution for He data in flight in comparison with GSI

7 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Search for Antihelium- N He /N He = 1.1·10 -6 Same spectrum for He, He (Ref. Phys. Lett. B461(1999) ) Model Independent Limit (95% C.L.) (from R min =1.6 GV to variable R max )

8 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Search for Antihelium-

9 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -CR Spectrum Measurements- At km above Earth’s surface studies with balloons for several decades. Important contributions to the understanding of the primary CR spectrum of charged particles and of atmospheric secondary particles Inner and outer radiation belts (1000 km-to-magnetosphere boundary) are studied by small size detectors on satellites Intermediate region (ToA-and-Inner radiation belt) contains low radiation levels. Before AMS the satellite-based detectors have not been sensitive enough for a systematic study of CR spectrum (except SAA )

10 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -CR Spectrum Measurements-

11 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Primary CR Spectra Measurements-

12 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Primary CR Spectra Measurements- Primary e - Spectrum e + /(e + +e - ) Ratio

13 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Primary CR Spectra Measurements-

14 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight -Primary CR Spectra Measurements-

15 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-

16 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO- Electron Spectra Positron Spectra

17 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO- To study the properties of second spectra of up/down going protons and leptons they have been traced through the magnetic field backward and forward for a t<10 s flight time or until they do not hit ToA (40km). Two distinct components are observed depending on the total travel time they before impact with ToA:  “Short-Lived” (<0.3 s): detected over all latitudes originated everywhere but at  M <0.3. Flux is independent on shuttle attitude  “Long-Lived” (>0.3 s):detected essentially at  M <0.3 originated in definite regions. Flux dependent on shuttle attitude

18 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO- Residence time vs. Energy for e + Residence time (s)

19 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-

20 B. Alpat, INFN Sezione di Perugia Adiabatic Invariants

21 B. Alpat, INFN Sezione di Perugia AMS-01 STS-91 Flight - Trapped Charged Particles on LEO- Left:Integral flux maps for e + (A)/e - (B) and Right:integral e + /e - ratio between  E  2.73 GeV L L

22 B. Alpat, INFN Sezione di Perugia AMS belts vs. Van Allen belts AMS belts:  High energy from ~ 1 GeV to ~ 10 GeV  Contains e+, e-, p, 3 He  e+ over e- dominance  Low L- shell  low altitude  Life time O(seconds) => Secondary production from CR interaction with atmosphere Van Allen belts:  Low energy from ~ 1 MeV to ~ 700 MeV  Contains e-, p  High L-shells  high altitude  Life time O(years)  Decays of neutrons produced in interactions of primary with the atmosphere (CRAND)  Solar wind induced magnetic storms

23 B. Alpat, INFN Sezione di Perugia AMS-02 on ISS 2004

24 B. Alpat, INFN Sezione di Perugia AMS-02 on ISS

25 B. Alpat, INFN Sezione di Perugia AMS-02 Physics on ISS

26 B. Alpat, INFN Sezione di Perugia AMS-02 as HE  ray detector

27 B. Alpat, INFN Sezione di Perugia Complementarity of , p, e + with AMS02 AMS will have the unique possibility to measure in space, with the same detector , p, e + spectra it will be the only experiment in space able to make an extensive test of the neutralino based dark matter scenario. No other detectors, planned or operating will be able to do this measurement _

28 B. Alpat, INFN Sezione di Perugia AMS-02 Physics on ISS (3 years) ElementsYield (or Sensitivity) (Now)Rigidity Range (GV) Physics e+ γ (~10 3 ) (~2000) Dark Matter (SUSY) He/He C/C 1/10 9 1/10 8 1/10 6 1/ Antimatter CPvsGUT, EW D,H 2 3 He/ 4 He 10 Be/ 9 Be % Astrophysics

29 B. Alpat, INFN Sezione di Perugia 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 search for antimatter and to study the energy spectra for primary and trapped CR fluxes AMS is approved by NASA to operate on the ISS for 3 years starting in 2004 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.


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