Search for Antiparticles in Cosmic Rays in Space and the ...philipvd/0806_hausseminar_PvD.pdf ·...

Philip von Doetinchem I. Phys. Inst. B, RWTH Aachen University

Hausseminar, Aachen –

6th of June 2008

Search for Antiparticles in Cosmic Raysin Space and the Earth’s Atmosphere

Search for Antiparticles in Cosmic RaysPh. von Doetinchem Hausseminar 08/06/06 – p. 2

Overview•

cosmic

ray

physics

in the

GeV-TeV

range

•

the

AMS-02 detector

for

the

ISS in Space:–

anticoincidence

counter

•

qualification

of hardware•

integration

•

analysis

–

prospects

for

AMS-02

•

the

PEBS detector

in Earth‘s

atmosphere:–

properties

of Earth‘s

atmosphere

and magnetic

field

–

simulation

of cosmic

ray

measurements

at the

Southpole–

prospects

for

PEBS


Particle & Astro

Physics

• particle

physics

& astrophysics

are

merging• use

particle

physics

methods

in astrophysics and get

input

to particle

physics

from

astrophysics

• important

observations

cry

for

explanations:– Dark

matter exists! What

is

the

nature? Supersymmetry, Kaluza-

Klein,…– Where

does

the

asymmetry

between

matter and antimatter in the

universe

come from?– …

WMAP 5 years


Cosmic Rays

kinetic Energy [GeV]-110 1 10 210

-1 s

r-1

s-2

m-1

GeV

Flu

x

-510

-410

-310

-210

-110

1

10

210

310

410

AMS-01 protons

AMS-01 helium

AMS-01 electronsHEAT 94/5 positrons

AMS-01 positrons

EGRET photons

IMAX antiprotons

Caprice 94 antiprotons

Caprice 98 antiprotonsBESS 95/97 antiprotons

BESS 02 antiprotons

= 441.641 MVΦsolar Modulation:

)αg

ald

ef 5

9927

8 / 5

9929

8(

protonheliumelectronpositronphotonantiproton

• learn

about

sources, acceleration, propagation, age, grammage

of matter, halo

size,…• good agreement

of models

in the

GeV-TeV

range

for

particles, some

unexplained features

in antiparticle/photon

spectra

AMS-02PEBS


Positrons & Antiprotons

• no primary

sources

for

positrons

and antiprotons

are

known• sensitive to new

physics: dark

matter annihilations

e.g. from

new

particles

in supersymmetric

or

Kaluza-Klein

Theories


Antihelium2 different appoaches

for

the

explanation

of the

baryon asymmetry:

• dynamically: large CP violation

is needed

• separation

of matter and antimatter in the

early

universe

measurement:• bound

on antihelium

gives

constraint

for

the

distance between galaxies

and antigalaxies

(NO(!) production

of antihelium

in the

matter universe

possible)

10-9

10-8

10-7

10-6

10-5

10-4

10-3

10-2

1 10 102

103

An

tih

eliu

m/H

eliu

m F

lux R

atio

(9

5%

C.L.)

Rigidity (GV)

(a) Buffington etal. 1981

(b) Golden etal. 1997

(c) Badhwar etal. 1978

(d) Alcaraz etal. 1998

(e) Sasaki etal. 2001

(a)

(b)(c)

(c)

(d)

(e)

AMS-02 3 Years


The AMS-02 Detector

artist

view

of AMS-02 on the

International Space

Station

> 2010

AMS-02 in the

clean room

@ CERN

3m7t


AMS-02 Overviewgoals of AMS-02:

•

precise spectroscopy of cosmic rays without interactions in the

atmosphere on the ISS• measurement/bounds on antimatter• indirect dark matter search

subdetectors:

Transition Radiation Detector (TRD)‏• classify particles by γ=E/m

Time of Flight (ToF)‏• trigger, velocity, dE/dx

Tracker + supraconducting

Magnet (1T)• track reconstruction, momentum, dE/dx

Anti-Coincidence Counter (ACC)‏• event selection next slide

Ring Image Cherenkov Detector (RICH) ‏• precise velocity mesaurement

Electromagnetic Calorimeter (ECal) ‏• shower shape and energy determination


Important Events for the ACC

ACC ACC

rejection of internal interactions rejection of external particles


ACC System•

small ACC inefficiency needed (<10-4) for measurement of antimatter with very clean single tracks

•

reduce trigger rate, fast detector (ns): e.g. south atlantic anomaly

WLS fiber Clear fiber

Charged particleCoupling

PMT

WLS fiberClear fiber

Coupling

Scintillator

PMT

PMT box,small B pos.

clear

fibers

scintillator

panels

2 panels

share

1 lower

and 1 upper

PMT

PMT box,small B pos.


Light Signals

PMT quantum efficiency

scintillator

with WLS fibers

attenuation of clear fiber


ACC Hardware Parts

panel side

PMT side

16 Y-shaped Toray clear fiber cables

16 Hamamatsu fine mesh PMTs,

B tolerant (0.5T 65% gain)

16 Bicron BC414 Scintillator Panels with inlaying Kuraray wave length shifting fibers


ACC Panel Production

finished

panel

curing

of glue

machining

of panel

glued

panel


adc200 400 600 800 1000

entr

ies

[#]

1

10

210

310

adc200 400 600 800 1000

entr

ies

[#]

1

10

210

310

410channel 0

channel 1

Panel Classification

cosmics LED

N pe=QCQLED

σ LED2

panel distribution

Entries 20Mean 18.71RMS 1.832

number of photo electrons[#]10 12 14 16 18 20 22 24

entr

ies

[#]

0

2

4

6

8

10

panel distribution

Entries 20Mean 18.71RMS 1.832

calculation of photo electron number:•

measurement of MOP with cosmics

•

calibration with LEDs implemented in panels

QC QLED test of all panels

material

photo elec.AMS-01

1.0cm

20

AMS-02

0.8cm

19


Coupling: WLS to Clear

Fiber

• acceptance

angle matching

of wavelength

shifting

fiber

and clear

fiber

is

important• WLS: wide

distribution

due

to reabsorption

is

also responsible

for

large attenuation

angle [deg]-60 -40 -20 0 20 40 60

entr

ies

[#]

0

100

200

300

400

500

600x Profile

y Profile

angle [deg]-60 -40 -20 0 20 40 60

entr

ies

[#]

0

100

200

300

400

500

600x Profile

y Profile

wavelength shifting fiber:

0.9dB/m

clear fiber: 0.15dB/m


Space Qualification -

PMTs

time [h]0 5 10 15 20 25 30 35 40 45

tem

per

atu

re [

deg

C]

-40

-20

0

20

40

60

Temperature requirements:operative: -30 -

+45 °C

non-operative: -35 -

+50 °C

TVT tank

PMTs

PMTs

PMTs did not changewithin 5% after Space

Qualification

random frequency spectrum: 3.3g


PMT Selection for Flight

time [s]-0.14 -0.12 -0.1 -0.08 -0.06 -0.04

-610×

amp

litu

de

[V]

-0.05

-0.04

-0.03

-0.02

-0.01

0

channel 26

channel 28

typical signal shape

classification with gain and p.e. number

mounting in light and glass dust tight box


Complete System Testtest of complete chain:

panel + clear fiber + PMT show good results

(mean: 16 photo electrons)


LED preintegration/system test0.5 0.6 0.7 0.8 0.9 1 1.1 1.2 1.3 1.4 1.5

entr

ies

[#]

0

5

10

15

20

25

30

35

40

45entries: 159

mean: 0.99

width: 0.08

Preintegration

successful preintegration:99 ±

8 %

LED test comparison (after/before) ‏


Inefficiency

Studies: Testbeam

-

Setup

test of slot and central region

slot

central

slot


Testbeam

–

Inefficiency Measurement

position [cm]0 5 10

sig

nal

rat

io

0.5

0.6

0.7

0.8

0.9

1

+ 1.0021.000 pos - 10.636cm

0.061cmratio =

highest ADC counts from both PMTs on one panel for each event

slot14.3 mm from slot

2.6 mm from slot

fit to MOP position

central

cent

ral

slot


Signal Ratios

position [cm]0 10 20 30 40

sig

nal

rat

io

0.65

0.7

0.75

0.8

0.85

0.9

0.95

1

1.05 pos+1-1ratio = -0.0076cm

channel 3 / channel 40 0.5 1 1.5 2 2.5 3

entr

ies

[#]

1

10

210

entries: 1121

mean: 0.99

RMS: 0.40

ratio of both PMT MOP signals on one panels vs. position

distribution of signal ratios at the central position

estimation of hit positioncentral


Signal Model

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

width [cm]-40 -30 -20 -10 0 10 20 30 40

len

gth

[cm

]

-40

-30

-20

-10

0

10

20

30

40

0.4

0.5

0.6

0.7

0.8

0.9

1

1.1

width [cm]-40 -30 -20 -10 0 10 20 30 40

len

gth

[cm

]-40

-30

-20

-10

0

10

20

30

40

model for relative signal behaviour of one PMT

model for relative signal behaviour for the highest

value of both PMTs

PMT

PMT

PMT


Flight Electronics2 branches

of signal

processing:

• fast veto

decision

for

level1 trigger

with

discriminator

threshold• charge

and time measurement

after

trigger

(ADC, TDC)


Flight

Electronics: Calibration

s]μdelay [0 5 10 15 20 25 30 35 40

AD

C c

ou

nts

[#]

0

100

200

300

400

500

600

700

800 60pC12pC2pC

, 5nFΩtest pulse, Gain 25, 1.2k

Threshold0 50 100 150 200 250

Vo

ltag

e [m

V]

0

10

20

30

40

50V = 0.20 thr+ 1.76

ADC counts [#]0 500 1000 1500 2000

char

ge

[pC

]

0

100

200

300

400

500

600

700

800

, 5nF, side AΩtest pulse, Gain 25, 1.2k

time delay scan to get to the maximum signal of the ADC

gauging of ADC charge measurement with test pulses: high resolution for small charges

calibration of thresholds for the discrimination in the TDC


Flight Electronics

ACC0 / ADC counts [#]0 50 100 150 200 250 300

AC

C1

/ AD

C c

ou

nts

[#]

0

50

100

150

200

250

300

-110

1

10

•

2 PMTs

(ACC0/1) connected to one panel

•

no event missed out of 10000 by using the highest of both values

3RMS of pedestal

ADC counts [#]0 100 200 300 400 500 600 700 800 900 1000

entr

ies

[#]

1

10

210

310

410 ACC 0

ACC 1

ACC0+WLS

ACC1+WLS


Isotropic Particle Distribution

•

beamtest: straight infall to panel

•

space: isotropic particle distribution leads to longer

path lengths in

scinitillator [deg]θangle 0 20 40 60 80

sig

nal

rat

io

1

2

3

4

5

6

isotropic particle toy MC distribution of travelled

paths in scintillator thickness: 0.8cm

lab measurement of rel. signal vs. angle:good agreement

with theory

theory


Inefficiency Model

• Data:

Mean inefficiency for one complete ACC

panel

with complete system test results and isotropic particle distribution and testbeam

electronics:

5⋅10-5

•

Simulation: use of testbeam

spectra with extrapolation to small values, system test, flight electronics, position measurements, isotropic particle distribution, smearing of signal values: 5⋅10-6

X position [cm]-40 -30 -20 -10 0 10 20 30 40

Inef

fici

ency

-810

-710

-610

-510

-410

-310

-210MC: LeCroy

MC: SFEA2

Y position [cm]-10 -5 0 5 10

Inef

fici

ency

-810

-710

-610

-510

-410

-310

-210TestbeamMC: LeCroy

MC: SFEA2

slot slot

central central


AMS-02 Cosmics: EventdisplayAMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008AMS Event Display Run 1210153173/ 76281 Wed May 7 11:43:06 2008

DAQ

Level1

Header

x y

z

Front

DAQ

Level1

Header

xy

z

Side

DAQ

Level1

Header

x y

z

Front

DAQ

Level1

Header

xy

z

Side

1.000 Coo=(-62.33,-20.61,-52.99) AntiC=-34.00 ±=-1.000β=5.98 Q= 1 φ=0.63 θ nan ± 1e+21 M= 0± Particle TofTrd No 0 Id=2 p= -1e+07


Event Selection

time of hit in TDC for 1 hit per eventrequire for selection at least one hit within 80ns of trigger

matching of TRD track with tracker:• at least

two tracker hits within 0.25cm•

one hit within 0.25cm in last layer before extrapolated hit position in ACC

| [cm]TR-hitTRD

tracker: |hit0 10 20 30 40 50 60

entr

ies

[#]

1

10

210

310

410

510

610

710entries: 8817918

effect of multiplexing in x direction

Tracker

layer

5 distance (Δx2+Δy2)1/2

trigger

noisenoise


AMS-02 Cosmics

cos(zenith)0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

entr

ies

[#]

1

10

210

310

410

510

610ACC: 13066

TRD: 4978989

zenith angles for all good TRD and for ACC events surviving all cuts

highest ADC value for each event surviving tracker cuts: no events below 30 (3RMS)

Inefficiency < 7.7⋅10-5

ADC counts [#]0 1000 2000 3000 4000

entr

ies

[#]

1

10

210

310

410entries: 13066


AMS-02 Cosmics: Signals

-110

1

10

[rad]φ-3 -2 -1 0 1 2 3

AD

C c

ou

nts

[#]

0

500

1000

1500

2000

2500

3000

3500

4000

entries: 12987

-110

1

10

[rad]φ-3 -2 -1 0 1 2 3

AD

C c

ou

nts

[#]

0

500

1000

1500

2000

2500

3000

3500

4000

entries: 9812

not very well configured: • mix of EM, QM and FM• different settings and conditions

upper PMTs lower PMTs

12 3

4

5

678


-210

-110

1

[rad]φ-3 -2 -1 0 1 2 3

z [c

m]

-100

-50

0

50

100

entries: 81

Position Matching: ACC/Track

5 6 7 8 1 2 3 4 -110

1

10

ACC sector [#]1 2 3 4 5 6 7 8

AC

C s

ecto

r fr

om

Tra

ck [

#]

1

2

3

4

5

6

7

8

entries: 81

position of hits below 30 very close to adjacent panel:• adjacent panels show normal signals • TRD/tracker matching not precise enough• scattering in detector

position of hits with small signals

no events missed out of 13000 ACC events

considering the complete ACC


Antihelium with AMS-02

larger angular acceptance of ACC

than TOF

• check for

the

ability

to measure

particles

between

triggers

with

the

ACC which

could

spoil

the

charge

determination

• toy

MC with

TOF, Tracker and ACC

with

isotropic

particle

distribution

and without

magnetic

field



external eventTOF trigger event

distance between hits is interesting for charge measurement efficiency

TOF

TOF



number of close hits0 1 2 3 4 5 6 7 8

pro

bab

ility

[%

]

-410

-310

-210

-110

1

10

210

310

|<0.05mACC-hitTOF

close hit: 0m<|hit |<0.05mACC-hitTOF

close hit: 0m<|hit

distance in tracker layers between TOF trigger events and external events

probabilty

for close hits (<5cm) not longer than 80ns from trigger @ 2kHz

external

hits

can

be

nearly

completlyexcluded

to spoil

charge

measurement

ext


Antiprotons with

TRD, TOF and Tracker

Energy [GeV]1.5 2 2.5 3 3.5 4 4.5 5

Ele

ctro

n R

ejec

tio

n

1

10

210-efficiencyp90%

Energy [GeV]0 50 100 150 200 250

Ele

ctro

n R

ejec

tio

n1

10

210

-efficiencyp70%

electron rejection from time resolution of TOF (100ps) due to different masses

electron rejection from TRD from Lorentz factor γ=E/m due to different masses


Antiprotons with

TRD, TOF and Tracker

Energy [GeV]1 10 210

]-2

m-1 s

-1sr

-1F

lux

[GeV

-710

-610

-510

-410

-310

-210

-110

1

10

210

310

410

AMS01 protonsIMAX antiprotonsCaprice 94 antiprotonsCaprice 98 antiprotonsBESS 95/97 antiprotonsBESS 02 antiprotonscombined antiprotons

, AMS, 1095 dayspp, AMS, 1095 days

conv. Galprop


]+/p

pA

nti

pro

ton

Fra

ctio

n [

-510

-410

-310

IMAXCaprice 98

Caprice 94

BESS 95/97

BESS 02

HeatPamela (preliminary)

AMS, 1095 days

AMS, sys. error

Galprop + DM

DM, DarkSUSY

conv. Galprop

= 1560 GeV0

= 262 GeV, m1/2m

= 00

>0, Aμ= 40, βtan

DM signal boost factor: 1.0

measurement over 3 years with:• acceptance = 0.4m2sr• 63% efficiency• 10% systematic errors to the knowledge of detector properties• tracker resolution is not important in this energy range (σp

=0.04%/GeV⋅p⊕1.5%)

good measurement of antiprotons without electromagnetic calorimeter possible


PEBS –

Cosmic

Rays in the

Atmosphere

PositronElectronBalloon

Spectrometer

detector

proposal:• cosmic

ray

measurements

@ North-

or

Southpole• balloon

in 40km altitude

in the

atmosphere

and magnetic

field

detector

properties:• flight

time: 100days (total)

• acceptance: 0.4m2sr• magnetic

field: 1T

• weight: < 2t


Analysis Scheme

PLANETOCOSMICS

produce spectra of galactic cosmic ray

GALPROPDarkSUSY

solar Modulationforce field approximation

isotropic distributionin 40km height

Earth’s magnetic field and atmosphere(IGRF, NRLMSIS00)

compare secondary muonswith BESS @ Ft. Sumner, TX

verify simulation

simulate at South Poleextract galactic fluxes

calculate errors


Air Shower• use

of program

package:

PLANETOCOSMICS

based on GEANT4

• atmospheric

model: NRLMSISE00

• magnetic

field: IGRF 2005

• detection

planes around

the Earth

• start particles

in 500km altitude

10GeV proton


Properties

of the

Atmosphere

Altitude [km]0 10 20 30 40 50 60 70 80

Tem

per

atu

re [

deg

Cel

siu

s]

-120

-100

-80

-60

-40

-20

0

20

Altitude [km]0 10 20 30 40 50 60 70 80

]2d

epth

[g

/cm

-210

-110

1

10

210

310

kinetic gas temperature of the atmosphere at latitude -75°,

December (Southpole)

depth (integrated density) of atmosphere for zenith angle =

0°, latitude -75°, December (Southpole)

10°C

3.7g/cm2


Radiation Lengths

cos(zenith)0 0.2 0.4 0.6 0.8 1

nu

mb

er o

f ra

dia

tio

n le

ng

th

0

0.5

1

1.5

2

2.5

number of crossed radiation lengths depends on zenith angle

distribution of crossed radiation lengths before 40km during

summer at Southpole

using an isotropic particle distribution


Magnetic Field


Geomagnetic Cut-off

azimuth [deg]0 50 100 150 200 250 300 350

zen

ith

[d

eg]

0

10

20

30

40

50

60

70

80

90

cut-

off

[G

V]

0

2

4

6

8

10

12

14

16

18

20

geomagnetic cut-off for particles with zenith angle = 0°

geomagnetic cut-off depends on zenith and azimuth at each

location

Ft. Sumner, Texas


BESS Muon

Data in Texas

Energy [GeV]1 10

]-2

m-1 s

-1sr

-1F

lux

[GeV

-210

-110

1

10

210237000 m, 4.7 g/cm

230000 m, 13 g/cm

2BESS 4.68 g/cm

2BESS 13.4 g/cm

good agreement

of simulated secondary muons

with BESS data

at Ft. Sumner

simulated angular distribution for muons

in 37km altitude

Simulation works, now

Southpole


Fluxes

in different Altitudes

integrated flux (1-130GeV): primary particles

integrated flux (1-130GeV): secondary particles


Detector Acceptance

cos(zenith)0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

]-1 s

-2m

-1F

lux

[sr

-710

-610

-510

-410

-310

-210

-110

1

10

210

310

410primary positrons, 40000m

secondary positrons, 40000m

)detαcos(0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 1

En

trie

s [#

]10

210

310

410

angular distribution of secondary and primary positrons

angular acceptance of PEBS works as filter on secondaries


Atmospheric

Attenuation

in 40 km

total antiprotons / generated antiprotons

total positrons / generated positrons

atmosphere

is

electromagnetically

much

more

effective


Detector Properties

/ GeVBeamE50 100 150 200 250

Ele

ctro

n R

ejec

tio

n F

acto

r

10

210

310 70% e-Eff. 2x8 Layer

80% e-Eff. 2x8 Layer


/ GeVBeamE50 100 150 200 250

Pro

ton

Rej

ecti

on

Fac

tor

10

210

310 70% e-Eff. 2x8 Layer


90% e-Eff. 2x8 Layer proton/positron rejection

from TRD

electron/antiproton rejection

from TRD

electron/positron rejection

from tracker

electron/antiproton rejection from TOF

σp

=0.194%/GeV⋅p⊕2.3%

Ecal

rejectionsp+/e+

and e-/p-: 5000 (70% Efficiency)

Energy [GeV]1.5 2 2.5 3 3.5 4 4.5 5

Ele

ctro

n R

ejec

tio

n

1

10

210-efficiencyp90%

Energy [GeV]50 100 150 200 250 300

- e

→+ eP

rob

abili

ty E

-1310

-1210

-1110

-1010

-910

-810

-710

-610

-510

-410

-310

-210

-110

1


Total Number of Particles


[#]

PE

BS

N

1

10

210

310

410

510

610

710

810

910

1010, PEBS, 100 daysptotal

, PEBS, 100 days+total p


[#]

PE

BS

N1

10

210

310

410

510

610

710

810

910

1010, PEBS, 100 days+total e

, PEBS, 100 days-total e

protons

and antiprotons electrons

and positrons


Composition


[%]

-210

-110

1

10

210

, PEBS, 100 daysptotal

altitude, PEBS, 100 dayspprim. altitude, PEBS, 100 dayspsec.

, PEBS, 100 days-wrong e

, PEBS, 100 days-μwrong , PEBS, 100 days-πwrong , PEBS, 100 days+wrong p


[%]

-210

-110

1

10

210

, PEBS, 100 days+total e

altitude, PEBS, 100 days+prim. e

altitude, PEBS, 100 days+sec. e

, PEBS, 100 days+wrong p

, PEBS, 100 days-wrong e

antiprotons positrons

secondaryantiprotons

muons

pions

primaryantiprotons

electrons

primarypositrons

secondarypositrons

electrons

protons

using

the

according

rejections

and efficiencies

for

each

type


Antiprotons


]-2

m-1 s

-1sr

-1F

lux

[GeV

-710

-610

-510

-410

-310

-210

-110

1

10

210

310

410

AMS01 protonsIMAX antiprotonsCaprice 94 antiprotonsCaprice 98 antiprotonsBESS 95/97 antiprotonsBESS 02 antiprotonscombined antiprotons

, PEBS, 100 dayspp, PEBS, 100 days

conv. Galprop


]+/p

pA

nti

pro

ton

Fra

ctio

n [

-510

-410

-310

IMAXCaprice 98

Caprice 94

BESS 95/97

BESS 02

HeatPamela (preliminary)

PEBS, 100 days

PEBS, sys. error

Galprop + DM

DM, DarkSUSY

conv. Galprop

= 1560 GeV0

= 262 GeV, m1/2m

= 00

>0, Aμ= 40, βtan


using

the

according

rejections

and efficiencies

for

each

typewith

systematic

errors

for

detectors

of 3% and 15% for

the

atmosphere

fluxes fraction


Positrons


]-2

m-1 s

-1sr

-1F

lux

[GeV

-710

-610

-510

-410

-310

-210

-110

1

10

210

310

410

AMS-01 electrons

AMS-01 positrons

HEAT 94/5 positrons

, PEBS, 100 days+e

, PEBS, 100 days-e

conv. Galprop


-+e+ e+ e

Po

sitr

on

Fra

ctio

n

-110 PEBS, 100 days

PEBS, sys. error

HEAT

AMS01

combined

Galprop + DM

DM, DarkSUSY

conv. Galprop

= 1560 GeV0

= 260 GeV, m1/2m

= 00

>0, Aμ= 40, βtan


using

the

according

rejections

and efficiencies

for

each

typewith

systematic

errors

for

detectors

of 3% and 15% for

the

atmosphere

fluxes fraction


Conclusion•

ACC system for AMS-02 works!–

scintillators, clear fibers, PMTs: good

–

flight electronics: good–

preintegration

done!

–

cosmic test of AMS-02–

good inefficiency of about 10-5

for antimatter

search•

PEBS prospects are promising!–

atmospheric and magnetic simulations work fine

–

good capabilities to measure positrons and antiprotons and Southpole

or Northpole

Search for Antiparticles in Cosmic Rays in Space and the ...philipvd/0806_hausseminar_PvD.pdf ·...

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