Title: Alpha Magnetic Spectrometer AMS on International Space Station ISS
1Alpha Magnetic Spectrometer (AMS) on
International Space Station (ISS)
- Behcet Alpat
- I.N.F.N. Perugia
- Frontier Detectors for Frontier Physics
- 8th Pisa Meeting on Advanced Detectors
- May 21-27, 2000 La Biodola, Isola dElba, Italy
2The AMS Physics
- To search for Antimatter (He,C) in space with a
sensitivity of 103 to 104 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.
3AMS-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 Z8, Rigidity (p/Z)
- Anticounters
- Veto stray trajectories and bckgnd particles from
magnet walls - Aerogel Threshold Cerenkov
- ? measurements (1?3 GeV/c) for better e/p
separation - Low Energy Particle Shielding (LEPS)
- Carbon fibre, shield from low energy (lt5MeV)
particles
4AMS-01 STS-91 Flight Results
G.F. ? 3000 cm2.sr MDR ? 400 GV Energy Range
100 MeV/nltEklt 300 GeV/n Electronics channels ?
70000 Power ? 1 kW
- ?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)
5AMS-01 on Discovery during STS-91 Flight
6AMS-01 STS-91 Flight Results (2)
- 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,N)
- Geomagnetic effects on cosmic ray
7AMS-01 STS-91 Flight Physics Results (1)
NHe/NHe 1.110-6 Same spectrum for He,
He (Ref. Phys. Lett. B461(1999)387-396)
Any Spectrum from He
8AMS-01 STS-91 Flight Physics Results (2)
(Ref. Phys. Lett. B472(2000)215-226)
9AMS on ISS ? AMS-02
10AMS-02 on ISS
11AMS-02 on ISS
12AMS-02 Superconducting Magnet (1)
13AMS-02 Superconducting Magnet (2)Critical
Parameters
- Nominal Bending Power 0.85 Tm2
- Stray field _at_ radius of 230 cm lt 15.2 mT
- Peak in coil 6.6 T
- N. of Coils 2 Dipoles, 20 racetracks
- Magnetic Torque 0.272 Nm
- Conductor NbTi wire, Aluminum stabilized
- Operating Temperature 1.8 K _at_ 20 mbar (2600 lt
superfluid Helium) - Operating Current 450 A
- Power 1.5 kW (peak, during ramp), 400 W
(maintenance) - Endurance 27 to 33 months (w cryocoolers)
- Weight about 3 tons (whole magnetic system)
- Dimensions 2.7 m of diameter and 1.5 m of max
height
14AMS-02 Synchrotron Radiation Detector
- Aim
- Identify the charge of TeV electrons and PeV
nuclei using their synchrotron radiation in the
earths magnetic field by observing synchrotron
photons (Ethr KeV and eV respectively) in
detector (2x3 m2). - Photons position, counting and energy
measurements give info on - Particles charge sign, estimation on primary
electron momentum hence distinguish electrons
from nuclei. - April 2001, a small stand-alone detector (PSRD)
will fly as secondary payload on the Space
Shuttle. - For this flight, 16 YAlO3Ce(YAP) scintillating
crystals of size 25x25x2 mm3 will be coupled
directly to Hamamatsu R5900U PMTs. - SRD will be installed on AMS-02 if PSRD will give
good results
15AMS-02 Transition Radiation Detector (1)
- (Straw Drift Tube System), Aim
- Non-destructive information for particle
identification in addition to electromagnetic
calorimeter - Identification of hadrons (?s against Ks and
ps) and electrons - Final goal is good e/h separation between 1-2
(TRthr) GeV to about 100 GeV (hadrons start to
radiate) - e/p Rejection 1.5 to 4 10-3 with ? 90?95
electron efficiency - 6 mm diameter, 1.3 to 2 m long straw tubes
- Radiators Foam (Airex) or (10 ?m or 16 ?m)
fibre (0.06 g/cm3) - Gas mixture Xe/CO2 80/20, gain ? 2.5 104
- Operating temperature interval 10 C to 25 C
(gradient ? 1 K) - Weight 484 kg (350 kg detector)
- Test beam with e? and p (3.5 to 15 GeV)
- Tests and studies are underway for the final
choice of radiator, gas mixture and GCPS, vacuum
properties of straw tubes, radiator
outgassing,mechanical stability etc.
16AMS-02 Time of Flight System (1)
- Aim
- Fast Trigger (L1) to the experiment
- ToF measurements of the particles w up/down
resolution _at_ 10-8 level - e/p separation up to about 1.5 GeV
- Absolute charge determination (in addition to
tracker) - Total Surface 8 m2
- Four layers each composed by 11cm wide (1cm
thick) scintillator paddles - Each paddle seen by 2 PMT at both ends
- Total PMT 224 (Hamamatsu fine-mesh tubes, space
qualified, operates in B of 1?3 kGauss, _at_ 2kV, 2
PMT/ counter-end) - The angle between the field and PMT axis should
be lt45 - Total weight 250 kg
- INFN Bologna
17AMS-02 Time of Flight System (2)
18AMS-02 Time of Flight System (3) (T.o.F.
Resolution from AMS-01)
19AMS-02 Tracker (1)
- 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 of
electronics channel and ? 800 W of power. - A complex detector, qualified for operation in
space, with its ? 6 m2 of active surface will be
the largest ever built before the LHC _at_ CERN.
20AMS-02 Tracker (2)
- Operating Temperature -10/25 C
- Power Dissipation on the Detector 1 W/ladder, in
total 192 ladders - dP/P ? 2 _at_ 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). - INFN Perugia
21AMS-02 Tracker (3)(from AMS-01)
22AMS-02 Tracker (4)
23AMS-02 Tracker (5)
24AMS-02 Tracker (6)
25AMS-02 Ring Imaging Cerenkov Detector (1)
- Aim
- High efficiency rejection of albedo particles for
momenta above threshold - Measurement of particle velocity, mass
determination (with P measurement from Tracker) - dM/MdP/P ?2 d?/?
- Isotope identification below masses up to A ?25
(10Be/9Be, 3He/4He etc.) and identification of
chemical elements up Z ? 26 (up to Tracker
rigidity limit) - High level redundancy for e/p separation
26AMS-02 Ring Imaging Cerenkov Detector (2)
- Acceptance ? 0.4 m2.sr
- Radiator (NaF) n1.15 (2 cm thick) or n1.34 (1
cm) - Light Yield (N?) ? 50
- PMTs are pixelized version of Hamamatsu R5900 (16
pixels, 0.45x0.45 cm2 each) - Goal is
- d?/ ? ? 0.1 , p1.7 to 7.3 GeV/c/amu (for
n1.15) - 9Be and 10Be separation w Mass Resolution of ?
0.2 up to 10 GeV - INFN Bologna and ASI
27AMS-02 Ring Imaging Cerenkov Detector (3)
28AMS-02 Ring Imaging Cerenkov Detector (4)
29AMS-02 Ring Imaging Cerenkov Detector (5)
30AMS-02 Electromagnetic Calorimeter (1)
- Aim
- e/h separation _at_ 10-4 level in 1 ? 1000 GeV range
- High energy ? detection w good angular and energy
resolution - Distinct signature for antinuclei
- Measurement of neutral (albedo) particles (?,n,n)
- Energy Resolution (Simul.) ? 6.1 ? 3.1 _at_
1 GeV - ?
4.4 ? 1.2 _at_ 10 GeV - ?
1.46 ? 0.2 _at_ 100 GeV - INFN Pisa
31AMS-02 Electromagnetic Calorimeter (1)
32AMS-02 Electromagnetic Calorimeter (2)
33AMS-02 Electromagnetic Calorimeter (3)
34AMS-02 DAQ System (1)
- Link Speed
- Max raw link speed is 100 Mbps
- Max raw data transfer rate is ? 10 Mbytes/sec
- Data transfer rate w overhead is ? 5 Mbytes/sec
- Input data rate
- Max event rate is ? 2 kHz
- Average data size is ? 2 Kbytes
- Max input data rate is ? 4 Mbytes/sec
- Total 20-24 crates , max input data rate from
each crate is ? 2 Kbytes/sec - Output data rate
- Max output data rate is 100 Mbps
- Two links for data transfer
- Further data reduction on board with Level-3
algorithm (Solutions DSP or PowerPC750 from
Lockheed Martin) - IEEE1355 (Space Wire) standard at all board and
crate level communications
35AMS-02 DAQ System (2)
36AMS-02 Physics on ISS (1)
37AMS-02 Physics on ISS (2)
38AMS-02 Physics on ISS (3)
39AMS-02 on ISS
40Conclusions
- 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 is being built for the launch with the UF4
during fall 2003 - 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.