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