The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia...
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Transcript of The Results of Alpha Magnetic Spectrometer (AMS01) Experiment in Space Behcet Alpat I.N.F.N. Perugia...
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
B. Alpat, INFN Sezione di Perugia
The AMS Physics
To search for Antimatter (He,C) in space with a sensitivity of 102 to 103 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, 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.
B. Alpat, INFN Sezione di Perugia
AMS-01 Configuration on STS-91 Flight
STS-91 Flight, June 2-12th, 1998• 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 (up to 3 GeV/c) for better e/p separation
• Low Energy Particle Shielding (LEPS):
• Carbon fibre, shield from low energy (<5MeV) particles
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)
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
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
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Search for Antihelium-
NHe/NHe = 1.1·10-6
Same spectrum for He, He(Ref. Phys. Lett. B461(1999)387-396)
Model Independent Limit (95% C.L.)(from Rmin=1.6 GV to variable Rmax)
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Search for Antihelium-
54
Model Dependent Limit
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -CR Spectrum Measurements-
At 30-40 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 )
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -CR Spectrum Measurements-
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Primary CR Spectra Measurements-
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Primary CR Spectra Measurements-
Primary e- Spectrum e+/(e++e-) Ratio
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Primary CR Spectra Measurements-
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight -Primary CR Spectra Measurements-
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-
Electron Spectra Positron Spectra
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
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-
Residence time vs. Energy for e+
Res
iden
ce ti
me
(s)
B. Alpat, INFN Sezione di Perugia
AMS-01 STS-91 Flight - Trapped Charged Particles on LEO-
B. Alpat, INFN Sezione di Perugia
Adiabatic Invariants
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 0.205 E 2.73 GeV
L L
30
002
02
/311653.0
//
m
mm
LB
BBBBSinSin
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, 3He 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
B. Alpat, INFN Sezione di Perugia
AMS-02 on ISS
2004
B. Alpat, INFN Sezione di Perugia
AMS-02 on ISS
B. Alpat, INFN Sezione di Perugia
AMS-02 Physics on ISS
B. Alpat, INFN Sezione di Perugia
AMS-02 as HE ray detector
B. Alpat, INFN Sezione di Perugia
Complementarity of , p, e+ with AMS02
AMS will have the unique possibility tomeasure 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
_
B. Alpat, INFN Sezione di Perugia
AMS-02 Physics on ISS (3 years)
Elements Yield (or Sensitivity)
(Now) Rigidity Range (GV)
Physics
e+
γ
108
500000
(~103)
(~2000)
0.1-300
0.5-100
0.1-200
Dark Matter (SUSY)
He/He
C/C
1/109
1/108
1/106
1/104
0.5-1000
0.5-1000
Antimatter
CPvsGUT, EW
D,H2
3He/4He10Be/9Be
109
109
2%
1-20
1-20
1-15
Astrophysics
p
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.