trento summary: antimatter dark matter search
TRANSCRIPT
Trento Summary:
Antimatter & Dark MatterSearch
Th. Kirn & Th. Siedenburg
Status Dark Matter Search
W. Wallraff
Hausseminar, November 9th 2001
Physics AC-I
Trento: Matter, Antimatter, Dark MatterHow to reach Trento by car
Along the A22 Brenner motorway and the S.S.12 Abetone and Brenner. The S.S.45bis, Gardesana occidentale from Brescia and the Gardesana orientale from Verona;from Milan the S.S.42 to Tonale and Mendola; from Venice the S.S.47 of Valsugana;from Vicenza the S.S.46, all converge on Trento.
Villa Tambosi
Physics AC-IKirn 1
II International Workshop on Matter,Antimatter and Dark Matter
ECT*, Villa Tambosi,Trento, October 29 and 30th
2001
PROGRAM:
FIRST DAY, October 29th:
8.00 - 9.00 Registration
MORNING SESSION : 9.00 - 13.00
Chairman: M. Panasyuk
Recent Measurements on Cosmic Rays Spectra and Composition
9.00 Welcome by ECT* Scientific Secretary, Prof. Renzo Leonardi
9.05 - 9.40 R. Battiston (Perugia): Status of AMS on the ISS
9.45 - 10.10 J. Casaus (CIEMAT): Review of precision measurements on high energy hadrons
10.15 - 10.40 B. Bertucci (Perugia): Review of precision measurements on high energy leptons
10.45 - 11.00 Coffee break
11.00 - 11.25 P. Zuccon (Perugia): FLUKA simulation of the interaction of high energy CR with theatmosphere
11.30 - 11.55 T. Sanuki (Tokyo): Review on balloons muon measurements in the atmosphere
12.00 - 12.25 M. Gibilisco (ECT*): An analytical solution of the cosmic rays transport equation in the presence of the geomagnetic field
12.30 - 12.55 A. Sakharov (ETHZ): Macroscopically large antimatter regions in the Universe
13.15 Lunch (Villa Tambosi)
AFTERNOON SESSION : 14.30 - 18.30
Chairman: G. Battistoni
Interaction of Cosmic Rays with the Earth Geomagnetic Field
14.30 - 14.55 E. Fiandrini (Perugia): Trapped leptons measurement by AMS
Physics AC-IKirn 2
15.00 - 15.25 M. Buenerd (Grenoble): Secondary atmospheric particle populations at balloon andsatellite altitudes
15.30 - 15.55 D. Heynderickx (Belgium): Review on modelling of radiation belts
16.00 - 16.15 Coffee break
16.15 - 16.40 M. Casolino (Roma2): Review on NINA-1 and NINA-2 results
16.45 - 17.10 V. Mikhailov (Moscow): Low Energy Electrons and Positrons with Maria2 instrument
17.15 - 17.40 M. Panasyuk (MSU, Moscow): Review on anomalous trapped CR belts
17.45 - 18.10 M. Durante (Napoli): Review on biological implications of recent measurements oftrapped CR on LEO
18.15 - 18.40 A. Masiero (SISSA): Neutrinos and cosmology today
20.00 Social Dinner (Ristorante ‘Orso Grigio’)
SECOND DAY, October 30th:
MORNING SESSION : 9.00 - 13.00
Chairman: F. Cervelli
Recent Developments on atmospheric neutrinos
9.00 - 9.25 M. Shiozawa (ICRR, Tokyo): Review of experimental results on cosmic rays neutrinos
9.30 - 9.55 M. Vietri (Roma3): Extreme Energy Cosmic Rays and their sources and neutrinoastronomy
10.00 - 10.25 T. Stanev (Bartol): State of the art in calculations of the atmospheric neutrino flux
10.30 - 10.45 Coffee break
10.45 - 11.10 V. Plyaskine (ITEP): A recent new atmospheric neutrinos calculation
11.15 - 11.40 G. Battistoni (Milano): Calculation of secondary particle production in atmosphere andhadronic interaction
11.45 - 12.10 F. Vissani (LNGS): Massive neutrinos and theoretical developments
12.15 - 12.40 F. Cei (Pisa): Supernovae neutrinos (experimental status)
13.00 Lunch (Villa Tambosi)
AFTERNOON SESSION : 14.30 - 18.30
Chairman: B. Bertucci
Dark matter and gamma rays
14.30 - 14.55 P. Ullio (SISSA): Review of CR and Dark Matter Searches
15.00 - 15.25 P. Giommi (ASI SDC): Review of previous X-rays missions
15.30 - 15.55 N. Produit (Versoix): INTEGRAL, a gamma ray observatory
16.00 - 16.15 Coffee break
16.15 - 16.40 M. Tavani (Milano): Theoretical review on physics with gamma rays
16.45 - 17.10 M. Pohl (Geneva): Gamma physics with AMS
17.15 - 17.40 V. Choutko (MIT): AMS background studies for positrons and gamma rays
17.45 - 18.10 A. Morselli (Roma2) : Dark Matter Search with gamma rays with EGRET and GLAST
Physics AC-IKirn 3
Antimatter Search
Physics AC-IKirn 4
Composition and Energy Spectrum of
Cosmic Rays
Relative abundance of particles, elements and isotpesis related to:
• Primordial nucleosynthesis for the particles createdjust after the Big-Bang:γ, p, e, D,He4,He3, Li7
• Astrophysical sources accelerating primaries:e, p,He, C, O, Fe
• Interactions with interstellar gas create secondaries:e±, p, p, Li, Be,B
• propagation described by Leaky Box model
103 / s
1 / d
1 / min
1 / y
10-6
10-3
103
10-18
Inte
nsi
ty [
m-2
s-1sr
-1eV
-1]
Energy/Nucleon
p
He
e+ + e-
γ
AM
S rate
[GeV]
10-12
100
Physics AC-IKirn 5
Direct Antimatter Search
• p:
- Measurements do not provide evidence for extraga-lactic antimatter
- p-flux near earth can be explained mainly by secondaryinteractions of cosmic rays
10-3
10-2
10-1
10-1
1 10
Kinetic Energy (GeV)
p– f
lux
(m-2
sr-1
sec-1
GeV
-1)
1
1
Bottino2
2
Bergstrom3
3
Biebar4
4Mitsui λ(R,β)
55
Mitsui λ(R)
BESS(95+97)BESS(93)IMAXCAPRICE
Cosmic Ray P–
10-6
10-5
10-4
10-3
10-1
1 10
Kinetic Energy (GeV)
p–/p
rat
io
BESS(95+97)BESS(93)CAPRICEGolden et al.Bogomolov et al.Buffington et al.IMAXPBARLEAPMASS2
Physics AC-IKirn 6
Direct Antimatter Search
• antinucleon:
→ Discovery of antinucleus (He) ⇒ evidence for cos-mologically significant amounts of antimatter
→ Discovery of C ⇒ antistars
Presently, no antinucleus with Z ≥ 2 has ever beenfound in cosmic radiation
- ASM-01 98: He/He < 1.1 · 10−6; R < 100GV
- BESS 93-98: He/He < 1.0 · 10−6; R < 16GV
Physics AC-IKirn 7
AMS01 STS-91 Precursor Flight
Honeycomb
Silicon Wafers
Honeycomb
Computers
PhotomultipliersAerogel
Magnet
lectronics
Foam
Scintillators Low Energy Particle ShieldV
eto
Co
un
ters
^
z
yxP
erm
anen
t M
agn
et
Nd
-Fe-
B:
46 M
GO
e
1mCerenkov
Aerogel
TrackerPlanes
T1T2
T3
T4
T5T6
S3
S4
S2
S1TOF Layers
Particle TrajectoryLow Energy Particle Shields
AC
C
B=0.15T
• STS91 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
Physics AC-IKirn 8
AMS01 Results
Maximum rigidity (p/Z) depends on magnetic latitudeProton Flux
Kinetic Energy (GeV/N)
Flux
(Par
ticle
s/s/
MeV
)
θM < 0.3
0.3
< θ M
< 0
.40.
4 <
θ M <
0.5
0.5
< θ M
< 0
.6
0.6
< θ M
< 0
.7
0.7
< θ M
< 0
.80.8
< θ M
< 0
.9
0.9
< θ M
< 1
.0
1.0
< θ M
< 1
.1
θM > 1.1
10-7
10-6
10-5
10-4
10-3
10-2
10-1
1
10-1
1 10 102
Physics AC-IKirn 9
AMS01 Results
Eve
nts
1
10
10 2
10 3
10 4
10 5
-150 -100 -50 0 50 100 150
HeHe2.86×106 events0 events
Sign×Rigidity GV
AMSSTS - 91
Published Conservative Limits
Rigidity (GV)
Antim
atte
r/Mat
ter U
pper
Lim
it 9
5% C
L Z=
2
Smoot et al. (1975)
Buffington et al. (1981)
Golden et al. (1997)
BESS 1993-1995
AMS 1998
10-6
10-5
10-4
10-3
1 10 102
Physics AC-IKirn 10
AMS01 Results
Li
Be
B
C
N
∆ETracker (MIPS)
Eve
nts
0
200
400
600
800
1000
1200
1400
10 15 20 25 30 35 40 45
10-4
10-5
10-3
3 10 70
Rmin=1.6 GV
An
tiM
att
er/
Ma
tte
r U
pp
er
Lim
it
RmaxGV
Excluded
AMSSTS - 91
2 < |Z| < 8
Rigidity (GV)
Antima
tter/Ma
tter Up
per Lim
it 95%
CL Z>
2
Golden et al. (74)
Smoot et al. (75)
Smoot et al. (75)
AMS 98
10-5
10-4
10-3
10-2
1 10 102
Physics AC-IKirn 11
AMS02 – A Particle Spectrometer for ISSHow 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 yearsTRD Particle ID & 3D tracking20 layers fleece + Xe/CO25248 channels 6mm straw-tubes
p+/e+ < 10−2 (10 - 300 GeV)
TOF 1,2 Trigger σt≈125ps
Anticoincidence (Veto) counter
Silicon strip trackerwith internal laser alignment6 m2 in 3 double + 2 single xy layers1σ charge separation up to 1TV
Superconducting Magnet (ETH)B = 0.9T V = 0.6m3
TOF 3,4 1.3m distance to TOF 1,2p+/e+ > 3σ below 2 GeV
PFRICH AGL(+NaF) Radiatorfor A≤27 and Z≤28separation > 3σ from 1-12 GeV
ECAL 3D sampling lead/scint.-fibrewith p-E matching and shower-shape
p+/e+ < 10−4 (10 - 300 GeV)
Physics AC-IKirn 12
AMS02 Expectations
AMS01 statistics ×103 momentum reach ×6
010-1
102
103
104
105
106
107
108
109
1
10
-200 200 400 600 800 1000 1200 1400-1400
~109 eventsReg
ion
of
anti
mat
ter
(He)
Statistics /GV/c
AMS on ISS (search for antimatter)
Helium
–
Yie
ld in
GV
/c in
terv
als,
for
3 ye
ars
on
ISS
AM
S-0
1
1·109 He 1 - 1400 GV
3·106 p+ > 1 TeV1·107 e− > 10 GeV
Physics AC-IKirn 13
AMS02 Expectations
10-1
1
10
10 2
10 3
10 4
10 5
0 1000200 400 600 800GeV/c
Antiprotons
AMS on ISS
AM
S-0
1
106 events Energy > 5 GeV
(Search for dark matter)
Yie
ld in
GeV
/c in
terv
als,
for
3 ye
ars
on
ISS
10 2
10 3
10 4
10 5
10 6
10 7
10 8
10 9
10 10
0GeV/c
1000 2000 3000
Protons
Energy > 1 TeV
AM
S-0
1
~3 x 106 events
(extreme high energy cosmic rays)
Yie
ld in
GeV
/c in
terv
als,
for
3 ye
ars
on
ISS
10-1
1
10
10 2
10 3
10 4
10 5
10 6
10 7
10 8
0 1000 2000 3000GeV/c
Electrons~107 7 events
AMS on ISS
AM
S-0
1
Ener Energy gy > 10 GeV > 10 GeV
(Search for dark matter)
Yie
ld in
GeV
/c in
terv
als,
for
3 ye
ars
on
ISS
1
10
10 2
10 3
10 4
10 5
0 50-50 200 250100 300150GeV/c
Positrons4 x 104 x 106 6 events
AM
S-0
1
Ener Energy gy > 5 GeV > 5 GeV
Yie
ld in
GeV
/c in
terv
als,
for
3 ye
ars
on
ISS
AMS on ISS(Search for dark matter)
Physics AC-IKirn 14