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

physics

in the

GeV-TeV

AMS-02 detector

ISS in Space:–

anticoincidence

counter

qualification

of hardware•

integration

analysis

prospects

AMS-02

PEBS detector

in Earth‘s

atmosphere:–

properties

of Earth‘s

atmosphere

and magnetic

simulation

of cosmic

measurements

at the

Southpole–

prospects

Particle & Astro

Physics

• particle

physics

& astrophysics

merging• use

particle

physics

methods

in astrophysics and get

to particle

physics

astrophysics

• important

observations

explanations:– Dark

matter exists! What

nature? Supersymmetry, Kaluza-

Klein,…– Where

asymmetry

between

matter and antimatter in the

universe

come from?– …

WMAP 5 years

Cosmic Rays

kinetic Energy [GeV]-110 1 10 210

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:

protonheliumelectronpositronphotonantiproton

• learn

sources, acceleration, propagation, age, grammage

of matter, halo

size,…• good agreement

of models

in the

GeV-TeV

particles, some

unexplained features

in antiparticle/photon

spectra

AMS-02PEBS

Positrons & Antiprotons

• no primary

sources

positrons

and antiprotons

known• sensitive to new

physics: dark

matter annihilations

e.g. from

particles

in supersymmetric

Kaluza-Klein

Theories

Antihelium2 different appoaches

explanation

of the

baryon asymmetry:

• dynamically: large CP violation

is needed

• separation

of matter and antimatter in the

universe

measurement:• bound

on antihelium

constraint

distance between galaxies

and antigalaxies

(NO(!) production

of antihelium

in the

matter universe

possible)

1 10 102

Rigidity (GV)

(a) Buffington etal. 1981

(b) Golden etal. 1997

(c) Badhwar etal. 1978

(d) Alcaraz etal. 1998

(e) Sasaki etal. 2001

(b)(c)

AMS-02 3 Years

The AMS-02 Detector

artist

of AMS-02 on the

International Space

Station

> 2010

AMS-02 in the

clean room

@ CERN

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

WLS fiberClear fiber

Coupling

Scintillator

PMT box,small B pos.

fibers

scintillator

panels

2 panels

1 lower

and 1 upper

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

curing

of glue

machining

of panel

adc200 400 600 800 1000

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

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

AMS-02

Coupling: WLS to Clear

• acceptance

angle matching

of wavelength

shifting

and clear

important• WLS: wide

distribution

to reabsorption

also responsible

large attenuation

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

600x Profile

y Profile

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

600x Profile

y Profile

wavelength shifting fiber:

0.9dB/m

clear fiber: 0.15dB/m

Space Qualification -

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

Temperature requirements:operative: -30 -

+45 °C

non-operative: -35 -

+50 °C

TVT tank

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×

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

45entries: 159

mean: 0.99

width: 0.08

Preintegration

successful preintegration:99 ±

LED test comparison (after/before) ‏

Inefficiency

Studies: Testbeam

test of slot and central region

central

Testbeam

Inefficiency Measurement

position [cm]0 5 10

+ 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

Signal Ratios

position [cm]0 10 20 30 40

1.05 pos+1-1ratio = -0.0076cm

channel 3 / channel 40 0.5 1 1.5 2 2.5 3

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

width [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

Flight Electronics2 branches

of signal

processing:

• fast veto

decision

level1 trigger

discriminator

threshold• charge

and time measurement

trigger

(ADC, TDC)

Flight

Electronics: Calibration

s]μdelay [0 5 10 15 20 25 30 35 40

800 60pC12pC2pC

, 5nFΩtest pulse, Gain 25, 1.2k

Threshold0 50 100 150 200 250

50V = 0.20 thr+ 1.76

ADC counts [#]0 500 1000 1500 2000

, 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

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

410 ACC 0

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

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

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

-210MC: LeCroy

MC: SFEA2

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

-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

Level1

Header

Level1

Header

Level1

Header

Level1

Header

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

710entries: 8817918

effect of multiplexing in x direction

Tracker

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

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

410entries: 13066

AMS-02 Cosmics: Signals

[rad]φ-3 -2 -1 0 1 2 3

entries: 12987

[rad]φ-3 -2 -1 0 1 2 3

entries: 9812

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

upper PMTs lower PMTs

[rad]φ-3 -2 -1 0 1 2 3

entries: 81

Position Matching: ACC/Track

5 6 7 8 1 2 3 4 -110

ACC sector [#]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

ability

to measure

particles

between

triggers

ACC which

charge

determination

• toy

MC with

TOF, Tracker and ACC

isotropic

particle

distribution

and without

magnetic

external eventTOF trigger event

distance between hits is interesting for charge measurement efficiency

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

|<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

nearly

completlyexcluded

to spoil

charge

measurement

Antiprotons with

TRD, TOF and Tracker

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

210-efficiencyp90%

Energy [GeV]0 50 100 150 200 250

-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

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

, AMS, 1095 dayspp, AMS, 1095 days

conv. Galprop

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

>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

measurements

@ North-

Southpole• balloon

in 40km altitude

in the

atmosphere

and magnetic

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

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

December (Southpole)

depth (integrated density) of atmosphere for zenith angle =

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

3.7g/cm2

Radiation Lengths

cos(zenith)0 0.2 0.4 0.6 0.8 1

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

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

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

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

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

electromagnetically

effective

Detector Properties

/ GeVBeamE50 100 150 200 250

310 70% e-Eff. 2x8 Layer

80% e-Eff. 2x8 Layer

/ GeVBeamE50 100 150 200 250

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

=0.194%/GeV⋅p⊕2.3%

rejectionsp+/e+

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

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

210-efficiencyp90%

Energy [GeV]50 100 150 200 250 300

→+ eP

Total Number of Particles

1010, PEBS, 100 daysptotal

, PEBS, 100 days+total p

1010, PEBS, 100 days+total e

, PEBS, 100 days-total e

protons

and antiprotons electrons

and positrons

Composition

, 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

, 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

primaryantiprotons

electrons

primarypositrons

secondarypositrons

electrons

protons

according

rejections

and efficiencies

Antiprotons

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

, PEBS, 100 dayspp, PEBS, 100 days

conv. Galprop

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

>0, Aμ= 40, βtan

according

rejections

and efficiencies

typewith

systematic

errors

detectors

of 3% and 15% for

atmosphere

fluxes fraction

Positrons

AMS-01 electrons

AMS-01 positrons

HEAT 94/5 positrons

, PEBS, 100 days+e

, PEBS, 100 days-e

conv. Galprop

-+e+ e+ e

-110 PEBS, 100 days

PEBS, sys. error

combined

Galprop + DM

DM, DarkSUSY

conv. Galprop

= 1560 GeV0

= 260 GeV, m1/2m

>0, Aμ= 40, βtan

according

rejections

and efficiencies

typewith

systematic

errors

detectors

of 3% and 15% for

atmosphere

fluxes fraction

Conclusion•

ACC system for AMS-02 works!–

scintillators, clear fibers, PMTs: good

flight electronics: good–

preintegration

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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