Präzisionsmessungen der kosmischen Höhenstrahlung im Weltraum

Präzisionsmessungen der
kosmischen Höhenstrahlung
im Weltraum
Das AMS Experiment auf der
Internationalen Raumstation ISS
für die AMS-Kollaboration
Th. Kirn
I. Phys. Institut RWTH Aachen
Leipzig, 18. März 2002
Physics
AC-I
The AMS Detector
• AMS02 on ISS
• Cosmic Particle Spectroscopy
• AMS01 Results
• AMS02
• Conclusion
TRD
Veto
Counter
Tracker
TOF
3,4
USS II
He Vessel
1,2
Magnet
TOF
Vacuum
Case
Height: 3.50 m
Width: 2.30 m
Weight: 7 t
PFRICH
ECAL
Physics
AC-I
Th. Kirn,
1
ISS - an experimental platform
AMS02 on ISS

• Mean altitude 400 km 


• in orbit for 3 years


2

• acceptance 0.5 m sr
Physics
AC-I
=⇒ Cosmic Particle
Spectroscopy
Th. Kirn,
2
Experiments in Space
New environment for HEP experiments
• Acceleration during start and
landing; Design Goal up to 9g
• Operation in vacuum
• Temperature variations
−150 - +30 ◦C
• Deposition limits on ISS
< 10−14 g/s/cm2
• Weight limited to 14000 lbs
• Power consumption limited to 2kW
• Single Powersupply at 120 V
• Datarate 1 Mbyte/s via 1 datalink
=⇒ Cosmic Particle Spectroscopy
Physics
AC-I
Th. Kirn,
3
-1
p
-6
-2 -1
-1
10
10
γ
-12
3
10
/s
1/min
1/d
-18
10
e+
10
-3
p+-Contamination:
≤ 10−2
AC-I
+
0
1/y
e3
10
10
Energy/Nucleon [GeV]
flux ratio in orbit:
p+/e+ ≈ 104
Physics
He
AMS rate
Intensity [m s sr eV ]
Cosmic Particle Spectroscopy









⇒ p+-rejection > 106
Th. Kirn,
4
AMS Physics Goals
• Dark Matter Search ⇒ e+-Spectroscopy
=⇒ Cosmic-ray spectroscopy
with highest-precision in
Particle identification
p+-rejection > 106 to 300 GeV
• Matter-Antimatter Symmetry ⇔ Antimatter Search
He: cosmic antimatter
C: antimatter stars
Physics
AC-I
∆p/p < 30%
to 1000 GeV
Th. Kirn,
5
AMS01 STS-91 Precursor Flight
Particle Trajectory
Low Energy Particle Shields
TOF Layers
S1
Honeycomb
ergy Pa
rticle S
hield
S2
lectronics
Honeycomb
Computers
Tracker T1
Planes T2
T3
ACC
1m
Veto Counters
Foam
Permanent Magnet
Silicon Wafers
B=0.15T
T4
T5
T6
Nd-Fe-B: 46 MGOe
Low En
Scintillators
Magnet
S3
S4
Aerogel
Photomultipliers
z^
x^
Aerogel
Cerenkov
y^
• STS-91 2-11 June 1998
Shuttle Discovery
• Mean altitude 370 km
• 90 min orbit inclined at 51.7◦
• Trigger-rate 100-700 Hz
• Recorded 108 events in 100 h
P h y s ic s
A C -I
Th. Kirn,
6
AMS01 Results
M a x im u m
rigidity (p/Z) d e p e n d s o n magnetic l a t i t u d e
Primary + Secondary Proton Flux
θM > 1.1
-1
0.5 < θM < 0.6
-6
10
θM < 0.3
0.4 < θM < 0.5
0.3 < θM < 0.4
-5
10
0.7 < θM < 0.8
-4
10
0.6 < θM < 0.7
-3
10
0.8 < θM < 0.9
-2
10
0.9 < θM < 1.0
10
1.0 < θM < 1.1
Flux(Particles/s/MeV)
Primary Proton Flux
1
-7
10
10
-1
1
10
10
Kinetic Energy (GeV/N)
P h y s ic s
A C -I
2
Full Geant simulation of
the earth magnetic field
lead to a detailed understanding of the measured
spectra
Th. Kirn,
7
Events
10
10
4
10
3
10
AMS
STS - 91
5
He
He
0 events
2.86×106 events
2
10
Antihelium/helium flux ratio
AMS01 Results
He/He limit (95% C.L.)
10-2
Smoot et al. (1975)
Evenson (1972)
Aizu et al. (1961)
Evenson (1972)
Smoot et al. (1975)
10-3
Badhwar et al. (1978)
Golden et al. (1997)
10-4
Buffington et al. (1981)
10-5
1/90
BESS
10-6
AMS ('98 STS91)
( 93, 94, 95, 97 and 98 flights)
Physics
AC-I
W. Wallraff
1
-150
-100
-50
0
50
100
Sign×Rigidity
150
GV
10-7
10-1
04-06-99
1
10
Rigidity (GV/c)
Assume He and He have the same spectrum then
- AMS-01 98: He/He < 1.1 · 10−6; R < 100 GV
- BESS 93-98: He/He < 1.0 · 10−6; R < 16 GV
Search for Antihelium in Cosmic Rays
Phys. Lett. B461 (1999) 387-396
Cosmic Protons
Phys. Lett. B490 (2000) 27-35
Protons in Near Earth Orbit
Phys. Lett. B472 (2000) 215-226
Helium in Near Earth Orbit
Phys. Lett. B494 (2000) 193-202
Leptons in Near Earth Orbit
Phys. Lett. B484 (2000) 10-22
50 AMS01 related papers submitted to ICRC
2001
P h y s ic s
A C -I
Th. Kirn,
8
AMS02 – A Particle Spectrometer for ISS
How to suppress proton background to 10−6 and
perform high statistic tracking up to 1 TV?
Large acceptance 0.5 m2sr in orbit for 3 years
TRD Particle ID & 3D tracking
20 layers fleece + Xe/CO2
5248 channels 6mm straw-tubes
p+ -rejection > 102 (10 - 300 GeV)
TOF 1,2 Trigger
σt≈125ps
Anticoincidence (Veto) counter
Silicon strip tracker
with internal laser alignment
6 m2 in 3 double + 2 single xy layers
1σ charge separation up to 1TV
Superconducting Magnet (ETH)
B = 0.9T
V = 0.6m3
TOF 3,4
1.3m distance to TOF 1,2
+ +
p /e > 3σ below 2 GeV
PFRICH AGL(+NaF) Radiator
for A≤27 and Z≤28
separation > 3σ from 1-12 GeV
ECAL 3D sampling lead/scint.-fibre
with p-E matching and shower-shape
p+ -rejection > 104 (10 - 300 GeV)
P h y s ic s
A C -I
Th. Kirn,
9
AMS-02
SilicononTracker
Physics
of AMS-02
the Space Station
1
Veto
RICH
Calorimeter
He
––
He
Helium Vessel
Tracker
Magnet Coils
Superconducting
Magnet
TOF
• 8 layers, pitch 110 µm,
∆ = 10µm
• sagitta @ 30 GeV 1 mm
e±
TRD
• largest particle physics
Si-tracker before the turn-on
He4, Be9, Be10 off LHC
e±, γ
To be installed
onSiISS
AMS-02
Detector Beam Test Results
late 2004, for Beam-Test
3-5 years Result (120 GeV µ)
10
3
σp ~ 8.5 µm
events
10
2
p side
10
1
-100
-80
-60
-40
-20
0
20
40
60
80
100
µm
Residual distribution of hits on the ladder with respect
to the position expected from the beam telescope.
P h y s ic s
A C -I
Th. Kirn,
10
AMS-02 Laser Alignment
Plane 1
[cm]
60
40
IR Laser Beams
0
20
simultaneous 2 D I R b e a m
Si ladders
0
50m
µ
B
transparent Si with
SiNx anti reflective coating
profile measurements
with double sided Si detectors
(x-pitch 208 µm, y-pitch 110 µm)
Physics AC-I
Plane 6
IR Laser
delivery system
observed
hit in plane 2
dy
dx
hit derived from fit
using all but plane 2
plane 1
stiff particle track
plane 2
plane 3
B
plane 4
plane 5
Laser beam
plane 6
P h y s ic s
A C -I
Th. Kirn,
11
AMS-02 ECAL
3D Sampling, 15 X0 of Pb + scintillating fibres
Shower ⇒
e±-energy
Physics of AMS-02 on the Space
Station
+
e
1
Fibres
Lead
e±
TRD
TOF
o = 1mm
Aluminium
Veto
RICH
He
––
He
Helium Vessel
Tracker
Magnet Coils
Superconducting
Magnet
PM on both Ends
s
He4, Be9, Be10
th
o
nb
e±, γ
Calorimeter
d
En
PM
o
p+-rejection > 104 (10 - 300 GeV)
1 super layer (18.5 mm thick)
To be installed on ISS
late 2004, for 3-5 years
Total: 9 super layers 15 X0:
12%
σ
= √ + 1.5%
E
E
P h y s ic s
A C -I
(E in GeV)
Th. Kirn,
12
Physics of AMS-02
on the
Space Station
AMS-02
TRD
1
e±
––
He
Veto
He
RICH
Helium Vessel
Superconducting
Magnet
Tracker
Magnet Coils
TRD
TOF
p+-rejection > 102 (10 - 300 GeV)
Chosen Configuration for 60 cm height:
20 Layers each existing of
• 22 mm fleece
• ∅ 6 mm straw tubes (Xe/CO2
He4, Be9, Be10Realisation:
(80/20))
HERAb/ATLAS
e±, γ
One of 20 Layers
Calorimeter
Fleece−Radiator
LRP 375 BK (ATLAS)
0.06 g/cm3
22 mm
TR− γ
To be installed on ISS
late 2004, for 3-5 years
6 mm
Xe/CO2
e+
p
+
e Data
+
e MC
p Data
10 4
p MC
-
-
10 3
10 2
10
1
P h y s ic s
A C -I
0
10
20
30
Etube in keV
Th. Kirn,
13
Straw Modules
Module: 16 tubes at 6mm ∅ with 30 µm W-Au wire
M u ltila y e r C a p to n tu b in g s
Capton wall
6µm Carbon polyimide
0.2 µm Aluminum
C F C lo n g itu d in a l a n d
tr a n s v e r s a l s tiffe n e r s
25µm Kapton film
5 µm Polyurethane
25µm Kapton film
P o ly c a r b o n a te
C e n tr ic a to r
0.2 µm Aluminum
S e a l S to p p e r
C u -T e
E n d p ie c e
6µm Carbon polyimide
C r im p C o n n e c to r
E le c tr o n ic B o a r d
6 lo n g itu d in a l s tiffe n e r s
S tr ip s a c r o s s e v e r y 1 0 c m
Vortrag:
Entwicklung und Bau des AMS-Übergangsstrahlungsdetektors
St. Fopp, T407.4, Do 14:45, HS7
P h y s ic s
A C -I
Th. Kirn,
14
AMS-02 TRD
Octagon and Bulkheads support 328 Modules
(L=86 to 201 cm) with 100 µm mech. accuracy
Upper/lower 4 layers
measure in bending plane
Middle 12 layers
measure in perpendicular
plane
Vortrag: Test des AMS TRD mit
Myonen aus der Höhenstrahlung
F. Dömmecke, T407.3, Do 14:30,
HS7
P h y s ic s
A C -I
Th. Kirn,
15
AMS-02 TRD
Gassystem (P,T controlled)
16 vertical
layers
Be
am
Proton-Rejection
4 horizontal
layers
3000
0
100
20 Layer Prototype
Vortrag:
Strahltestergebnisse für den
AMS-Übergangsstrahlungsdetektor
J. Orboeck, T407.5, Do
15:00, HS7
200
3000
2000
2000
1000
1000
0
0
100
P h y s ic s
A C -I
0
200
Beam Energy in GeV
Th. Kirn,
16
AMS02 Expectations
AMS01 statistics ×103
109
AMS on ISS
momentum reach ×6
(search for antimatter)
Helium
106
105
104
103
102
10
1
10-1
-1400 -200
AMS-01
107
–
Region of antimatter (He)
Yield in GV/c intervals, for 3 years on ISS
108
0
~109 events
200
400
600
800
1000
1200
1400
S ta tis tic s /G V /c
1·109 He
P h y s ic s
A C -I
1 - 1400 GV
Th. Kirn,
17
AMS02 Expectations
AMS on ISS
(extreme high energy cosmic rays)
(Search for dark matter)
10
7
10
6
10
5
10
4
10
3
10
2
~3 x 106 events
Energy > 1 TeV
AMS on ISS
1000
2000
(Search for
dark
G e V / matter)
c
10
8
10
7
10
6
10
5
10
4
10
3
10
2
~107 events
Ener
Energy
gy > 10 GeV
-1
10
2
106 events
Energy > 5 GeV
10
1
-1
AMS on ISS
(Search
dark 600
matter)
0
200 for400
800
1000
10
5
10
4
10
3
10
2
Positrons
4 x 106 events
Energy
Energy > 5 GeV
10
1
0
1000
2000
G e V /c
P h y s ic s
3
Antiprotons
G e V /c
10
10
10
3000
Electrons
1
4
10
AMS-01
Yield in GeV/c intervals, for 3 years on ISS
0
10
AMS-01
8
Protons
10
AMS-01
10
Yield in GeV/c intervals, for 3 years on ISS
9
Yield in GeV/c intervals, for 3 years on ISS
10
AMS-01
Yield in GeV/c intervals, for 3 years on ISS
10 10
5
A C -I
3000
-50
0
50
100
150
200
250
300
G e V /c
Th. Kirn,
18
Conclusion + Outlook
• AMS-02 will have the unique possibility to
measure in space, with the same detector
γ, p, e+- spectra + nuclei isotopes
• AMS-02 offers a world wide unique discovery
potential for new physics
• Operation of a modern particle physics detector in
space for 3 years is a technical challenge.
• AMS02 Assembly end of 2003
• Set for liftoff in Nov. 2004
P h y s ic s
A C -I
Th. Kirn,
19
P h y s ic s
A C -I
Th. Kirn,
20