DAMPE mission Introduction

Chinese Academy of Science

DAMPE International Collaboration Team

China Purple Mountain Observatory CASInstitute of High Energy of Physics CAS Institute of Modern Physics CASNational Space Science CenterCASUniversity of Science and Technology of China

SwissGeneva University

Italy INFN Sez di Perugia Perugia UniversityINFN Sez di Bari Bari University

DAMPE Observation

Electron2GeV-10TeVGamma-rays2GeV-10TeVProton and Heavy Ions30GeV-1000TeV

Scientific Objectives

Science Objectives Observation TargetsNearby Cosmic-ray Sources Electron spectrum in trans-TeV regionDark Matter Signatures in electrongamma energy

spectra in 10GeV ndash 10 TeV regionOrigin and Acceleration of Cosmic Rays

p-Fe above 30 GeV

Cosmic ndashray Propagation in the Galaxy

BC ratio up to several TeV n

Gamma-ray Transients Gamma-ray time profileGamma-ray Astronomy Gamma-ray mapping

High energy electron lost energy prop1E2

Local TeV electronsAge lt ~105 years Distance lt 1 kpcLocal TeV electrons Vela Monogem Cygnus Loop

Nearby Cosmic-ray SourcesTrans-TeV electron spectrum observation

Electron spectrum depending on Vela and Cygnus LoopKobayashi 12102813

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

DAMPE International Collaboration Team

China Purple Mountain Observatory CASInstitute of High Energy of Physics CAS Institute of Modern Physics CASNational Space Science CenterCASUniversity of Science and Technology of China

SwissGeneva University

Italy INFN Sez di Perugia Perugia UniversityINFN Sez di Bari Bari University

DAMPE Observation

Electron2GeV-10TeVGamma-rays2GeV-10TeVProton and Heavy Ions30GeV-1000TeV

Scientific Objectives

Science Objectives Observation TargetsNearby Cosmic-ray Sources Electron spectrum in trans-TeV regionDark Matter Signatures in electrongamma energy

spectra in 10GeV ndash 10 TeV regionOrigin and Acceleration of Cosmic Rays

p-Fe above 30 GeV

Cosmic ndashray Propagation in the Galaxy

BC ratio up to several TeV n

Gamma-ray Transients Gamma-ray time profileGamma-ray Astronomy Gamma-ray mapping

High energy electron lost energy prop1E2

Local TeV electronsAge lt ~105 years Distance lt 1 kpcLocal TeV electrons Vela Monogem Cygnus Loop

Nearby Cosmic-ray SourcesTrans-TeV electron spectrum observation

Electron spectrum depending on Vela and Cygnus LoopKobayashi 12102813

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

DAMPE Observation

Electron2GeV-10TeVGamma-rays2GeV-10TeVProton and Heavy Ions30GeV-1000TeV

Scientific Objectives

Science Objectives Observation TargetsNearby Cosmic-ray Sources Electron spectrum in trans-TeV regionDark Matter Signatures in electrongamma energy

spectra in 10GeV ndash 10 TeV regionOrigin and Acceleration of Cosmic Rays

p-Fe above 30 GeV

Cosmic ndashray Propagation in the Galaxy

BC ratio up to several TeV n

Gamma-ray Transients Gamma-ray time profileGamma-ray Astronomy Gamma-ray mapping

High energy electron lost energy prop1E2

Local TeV electronsAge lt ~105 years Distance lt 1 kpcLocal TeV electrons Vela Monogem Cygnus Loop

Nearby Cosmic-ray SourcesTrans-TeV electron spectrum observation

Electron spectrum depending on Vela and Cygnus LoopKobayashi 12102813

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Scientific Objectives

Science Objectives Observation TargetsNearby Cosmic-ray Sources Electron spectrum in trans-TeV regionDark Matter Signatures in electrongamma energy

spectra in 10GeV ndash 10 TeV regionOrigin and Acceleration of Cosmic Rays

p-Fe above 30 GeV

Cosmic ndashray Propagation in the Galaxy

BC ratio up to several TeV n

Gamma-ray Transients Gamma-ray time profileGamma-ray Astronomy Gamma-ray mapping

High energy electron lost energy prop1E2

Local TeV electronsAge lt ~105 years Distance lt 1 kpcLocal TeV electrons Vela Monogem Cygnus Loop

Nearby Cosmic-ray SourcesTrans-TeV electron spectrum observation

Electron spectrum depending on Vela and Cygnus LoopKobayashi 12102813

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

High energy electron lost energy prop1E2

Local TeV electronsAge lt ~105 years Distance lt 1 kpcLocal TeV electrons Vela Monogem Cygnus Loop

Nearby Cosmic-ray SourcesTrans-TeV electron spectrum observation

Electron spectrum depending on Vela and Cygnus LoopKobayashi 12102813

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Cosmic ndashray Propagation in the GalaxyBC ratio observation

BC ratio SecondaryPrimayCNO+ISMBNBNC propλescσCNOB

Propagation in the Galaxy

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

γ line

WIMPs-gte+e-

Dark MatterSignals in eampγ spectrum amp space distribution

γ ndashray Halo Cut-off in e+ and e-

These signals are smoking gun of dark matter particle

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Present Observation

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Gamma-ray line in Clusters

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

PAMELA 7 year e- Observation

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

PAMELA 7 year e+ Observation

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

AMS02 e+ fraction

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

AMS02 and Pamela e- spectrum

Blue dots AMS02Red Dots Pamela

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

AMS02 e-+e+ amp Pamela e- spectrum

Blue dots AMS02 total electronRed Dots Pamela e-

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Present status

Cosmic electronsNo Space Observation above TeVs Cosmic ray Proton and Heavy Ionsfrom TeV to PeV no direct element spectral measurementGamma-ray astronomy

There is a gap between space and ground observation (10s GeV -100s GeV)No High energy resolution observation in spaceDark matter particle

No proof

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

We need a new detector

Energy range gtTeVEnergy resolution better than 15Background Rejection above 105

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

DAMPE Mission

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Payload Overview

Measurement DetectorCharge Si-strip amp Scintillation HodoscopeDirection Si-StripeEnergy BGO Calorimeter (31 rl)Background Rejection

BGO Cal Plus Neutron detector

塑闪阵列探测器

硅阵列探测器

BGO量能器

中子探测器

X+Y层塑料闪烁体

六层硅片

七层X+YBGO

输出击中信号用于触发判选第1234小层BGO

输出击中信号用于触发判选

第11121314小层BGO

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

The DAMPE Detector Plastic Scintillator Detector

Silicon-Tungsten Tracker

BGO Calorimeter

Neutron Detector

W converter + thick calorimeter (total 33 X0) + precise tracking + charge measurement high energy γ-ray electron and CR telescope

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Comparison with AMS-02 and Fermi

22

DAMPE AMS-02 Fermi LATeγ Energy range (GeV) 5 - 104 01 - 103 002 - 300eγ Energy res100 GeV () 15 3 10eγ Angular res100 GeV (deg)

01 03 01

ep discrimination 105 105 - 106 103

Calorimeter thickness (X0) 31 17 86Geometrical accep (m2sr) (e) 029 006 015

bull Geometrical acceptance with BGO alone 036 m2srndash BGO+STK+PSD 029 m2srndash First 10 layers of BGO (22 X0) +STK+PSD 036 m2sr

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Plastic Scintillator Detector (PSD) Two layers (x and y) of plastic scintillation strips of 1cm thick 28 cm

wide and 82 cm long ndash Strip staggered by 08 cm fully covered area 82cmtimes82cm

Readout both ends with PMT use two dynode signals (factor ~40) to extend the dynamic range ndash FE ASIC VA160 with dynamic range up to 12 pC

Expected performancendash Position resolution ~6 mmndash Charge resolution 025 undash Dynamic range Z = 1 - 20

23IMP Lanzhou

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Silicon Tungsten Tracker (STK) 12 layers of silicon micro-strip detector 7 support trays

ndash Tray carbon fiber face sheet with Al honeycomb corendash Sensor 95 x 95 cm2 4 sensors bonded together to form a ladderndash 16 ladders on each face of the support tray x-view and y-view

bull Except top and bottom trays only one face has ladders Tungsten plates integrated in trays 2 3 4 counting from the top

ndash Total 143 X0 for photon conversion

UniGE INFN Perugia amp Bari IHEP Beijing

Detection area 76cm x 76cmConsider to reduce to 086X0

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

STK Silicon Sensor Silicon strip detectors produced by Hamamatsu Photonics

ndash 95 x 95 cm2 768 strips 121 microm pitch (AGILE geometry) ndash 320plusmn15 microm thick (AGILE 410 microm)

Two types of SSD being consideredndash Type A resistivity 3-8 kΩ Vfd 40-120 Vndash Type B resistivity 5-8 kΩ Vfd 10-80 V

30 Type A SSD deliveredndash Vfd 75-80 Vndash ltIleakgt ~150 nA max 280 nAndash 0 bad channels

81 Type B SSD deliveredndash 54 with Vfd 45-50 V 26 with Vfd 65-70 Vndash ltIleakgt ~170 nA max 400 nAndash 1 bad channels

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

STK Ladder Assembly Special jigs designed to assemble (align glue and bond) 4 sensors

on a TFH to produce a ladder ndash Specification align 4 sensors to 40 microm planarity to 50 microm

26Gig design and prototyping in progress

TevPA Irvine 26-290813Xin Wu

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

STK Support Tray 7 trays 3 with tungsten plates

ndash 22 kg of tungsten for trays with 2mm plates ndash CFRP side beams and corners to reduce total weight (~140 kg)

bull A quarter size tray with 2mm tungsten plates have been produced by Composite Design (a Swiss company) ndash Being mounted with ladders and will go through vibration and

thermal tests

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

BGO Calorimeter (BGO) bull 14-layer BGO hodoscope 7 x-layers + 7 y-layersndash BGO bar 25cmtimes25cm 60cm long readout both ends with PMT

bull Use 3 dynode (2 5 8) signals to extend the dynamic rangendash Charge readout VA160 with dynamic range up to 12 pCndash Trigger readout VATA160 to generate hit signal above threshold

bull Detection area 60cmtimes60cm

28

Total thickness 31X0

PMO USTC

Measure electronphoton energy with great precision

between 5 GeV - 10 TeV

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Neutron Detector

Size 60cmX60cmX2cmBoron density 54 PMT

Neutron detector rejection power depending on electron selection eff

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Expected Performance from Simulation

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Energy Resolution

Energy resolution for electrons as a function of energyData was generated by G4 with particle vertically impacted on the center of ECAL(can ignore lateral leakage)As shown in plots Leakage Correction can give a better resolution

Energy Resolution at 5TeV ~ 0035

UncorrectedMean=47909plusmn01314Sigma=40020plusmn00721

CorrectedMean=50019plusmn00334Sigma=17306plusmn00207

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Energy Linearity

Leakage Correction can also give a better linearity The gradient from 09592 to 09996 We wish it perfectly equal to 1

10TeV e Energy deposit=94TeV

10TeV e shower profile Only 03 energy leakage from bottom

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Angular resolution just from BGO

Angle resolution for electrons as a function of energy and angleWith the energy increasing and angle decreasing angle resolution became betterIn high energy[500GeV~] Θ68 can reach less than 1 degree (simulation result)In low energy[~200GeV] angle resolution is not so good STK will provide better resolution

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

e p seperation Shower development in BGO calorimeter

22 22 14

1 1 1 ~frac li li

i i lE E E Y Axis

= = =

= minussum sumsum2 ~RMS X Axisminus

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Shower Structure Parameter - FValue

2fracFValue E RMS= sdot

Electron protonEnergy Range [9001000] GeV 19963 165617F13lt20ampampF14lt15 19060 108Efficiency or False Rejection Rate

9548 00652(15e+03)

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

ep discrimination by neutron detector

Deposited Energy at time window [1510]micros in NDAs plot proton is obviously different with electron we can use this difference to discriminate electron and proton Selection criterion 3MeVResult Reject 90 proton while keeping 983 electrons

Neutron detector rejection power depending on electron selection eff

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Gamma FoV will be increased by side incident events

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

38Xin Wu

PSF depending on energy

DAMPE is discussing to use 3mm W in total instead of 5mm

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

39Xin Wu

γ-ray GF for converted photon

Note unconverted γ-ray at high energy can add to efficiency

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Exposure time

1 day 30 Days

360 Days

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Gamma-ray mapping by 30 days

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Gamma-ray Sensitivity

CrabCALET

DAMPEFERMI

LHASSO

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

DAMPE for gamma-ray line observation

Fermi 195 Weeks

~ 8σ

DAMPE 3 years

Simulated 14 TeV gamma-ray line from dark matter toward the Galactic center (300 lt l lt 60 |b| lt10 ) including the Galactic diffuse background for DAMPE 6 Months observationsThe annihilation cross-section is taken as ltσvgtγγ = 1times10minus25

cm3sminus1 with a NFW halo profile The distinctive line signature is clearly seen in the gamma-ray spectrum

Monochromatic gamma-ray signals from WIMP dark matter annihilation would provide a distinctive signature of dark matter if detected Since gamma-ray line signatures are expected in the sub-TeV to TeV region due to annihilation or decay of dark matter particles DAMPE with anexcellent energy resolution of 1 above 100 GeV is a suitable instrument to detect these signatures

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Heavy Ion observation

Energy resolution for nuclei

λINT X0(nominal incidence)

DAMPE 1610485791048579 3410485791048579

CREAM 05+07 20

AMS02 05 17

Requirements for calorimetrybull Proton interaction requires gt 05 λINTbull Energy Measurement at 100 TeV scalerequires confinement of the em core ofthe shower ie gt 20 X010485791048579

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Heavy Ion results

Proton spectrum to asymp 900 TeVHe spectrum to asymp 400 TeVnSpectra of C O Ne Mg Si to asymp 20 TeVnBC ratio to asymp 4-6 TeVnFe spectrum to asymp 10 TeVn

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

BC ratio (1 year)

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Expected electron spectrum (1yr) by Vela source

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Expected performance for γ and e

Range 2GeV-10TeV

Effective Area 03m210GeV

Field of View 28 sr

Geometry Factor 085m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Point source

Sensitivity85X10-11cm-2s-1

Range 2GeV-10TeV

Geometry Factor 03m2sr

Energy resolution 15100GeV

Angular resolution 01O10GeV

Proton Rejection 105

Gamma sepeartion 100

γ performance e performance

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

DAMPE Beam Test

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Beam Test Setup Scheme

12 Layer BGOCal

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Beam Pipe

Trigger Si_Strip

Micromegas detectors

DAMPE Calorimeter

Beam Line

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Calibration with proton MIP

Proton MIP spectrum from one single

readout

Fitting Function Gaussian convolution landau

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Energy Resolution

bull Energy Resolution can reach 079 250GeV

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Electron Energy Spectrum

p=148746GeVPi amp energy leakage

121

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Energy Linearity

Energy Deviation = (Ereco-Ebeam)Ebeam

The gradient is equalto 0885 which mainly caused by dead region

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Reconstructed Angle distribution

200GeV electron vertically injectionLeft X-Z projection Right Y-Z Projection

σxz = 04109deg σyz = 03604

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Angle Resolution δangle

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

ep discrimination

Shower development in 1112 BGO Layer Red dots e black dots p

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

ep seperation

11FValue

12FValue

e pTotal events 24556 540145energy[100120]GeV

15163 12668

F11lt14ampF10lt19 14462 5Eff 9538 00395

These results agree with simulation very well

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Present Status

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Vibration Test PlasticHodoscope

Neutron Detector

BGO Cal

Satellite

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

Phase-Camp D

June 2014 end of Phase CFlight Model will be finished end of

2014Launch date June 2015

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢

谢谢

• Slide Number 1
• DAMPE International Collaboration Team
• DAMPE Observation
• Scientific Objectives
• Slide Number 5
• Cosmic ndashray Propagation in the GalaxyBC ratio observation
• Dark MatterSignals in eampγ spectrum amp space distribution
• Present Observation
• Slide Number 9
• Gamma-ray line in Clusters
• Slide Number 11
• Slide Number 12
• AMS02 e+ fraction
• Slide Number 14
• Slide Number 15
• AMS02 e-+e+ amp Pamela e- spectrum
• Present status
• We need a new detector
• Slide Number 19
• Slide Number 20
• The DAMPE Detector
• Comparison with AMS-02 and Fermi
• Plastic Scintillator Detector (PSD)
• Silicon Tungsten Tracker (STK)
• STK Silicon Sensor
• STK Ladder Assembly
• STK Support Tray
• BGO Calorimeter (BGO)
• Neutron Detector
• Expected Performance from Simulation
• Energy Resolution
• Energy Linearity
• Angular resolution just from BGO
• Slide Number 34
• Shower Structure Parameter - FValue
• ep discrimination by neutron detector
• Gamma FoV will be increased by side incident events
• PSF depending on energy
• g-ray GF for converted photon
• Exposure time
• Gamma-ray mapping by 30 days
• Gamma-ray Sensitivity
• Slide Number 43
• Heavy Ion observation
• Slide Number 45
• BC ratio (1 year)
• Expected electron spectrum (1yr) by Vela source
• Expected performance for γ and e
• DAMPE Beam Test
• Beam Test Setup Scheme
• Slide Number 51
• Calibration with proton MIP
• Energy Resolution
• Electron Energy Spectrum
• Energy Linearity
• Reconstructed Angle distribution
• Angle Resolution angle
• ep discrimination
• ep seperation
• Present Status
• Vibration Test
• Phase-Camp D
• 谢谢