Understanding Cosmic Rays and Searching for Dark Matter with PAMELA
The CALET Mission for Detection of Cosmic Ray Sources and Dark Matter
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Transcript of The CALET Mission for Detection of Cosmic Ray Sources and Dark Matter
Sep. 14, 2007 TAUP07 1
The CALET Mission The CALET Mission for Detection of Cosmic Ray Sources and Dark Matterfor Detection of Cosmic Ray Sources and Dark Matter
Shoji Torii Shoji Torii for the CALET Collaborationfor the CALET Collaboration
Research Institute for Science and EngineeringResearch Institute for Science and EngineeringWaseda UniversityWaseda University
Sendai, JapanSendai, Japan TAUP 07 TAUP 07 Sep. 14th 2007 Sep. 14th 2007
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Member List (24 organizations, 74 members)Japan : 14 organizations 38 membersS. Torii(1), N. Hasebe(1), M.Hareyama(1), N.Yamashita(1), O.Okudara (1), S.Kodara(1), Y.Shimizu(1),M.Miyajima(1), T.Miyaji(1), J. Nishimura(2), T. Yamagami(2) , Y. Saito(2), H. Fuke(2), M.Takayanagi(2), H. Tomida(2), S. Ueno(2) , T. Tamura(3), N. Tateyama(3), K. Hibino(3), S.Okuno(3), T. Yuda(4), M.Shiomi(4), M.Takita(4), Y.Katayose(5), M.Shibata(5), K.Kasahara(6), K. Yoshida(6), S. Kuramata(7), M. Ichimura(7), T.Terasawa(8), Y. Ichisada(8), Y. Uchihori(9), H. Kitamura(9), H. Murakami(10), T. Kobayashi(11), Y. Komori(12), K. Mizutani(13), K.Munakata(14)
(1) Waseda University (2) JAXA/ISAS (3) Kanagawa University (4 IICRR, University of Tokyo(5) Yokohama National University (6) Shibaura Institute of Technology (7) Hirosaki University(8) Tokyo Institute of Technology (9) National Institute of Radiological Sciences (10) Rikkyo University(11) Aoyama Gakuin University (12) Kanagawa University of Human Services (13) Saitama University(14) Shinshu University
USA: 5 organizations 14 membersNASA/GSFC: R.E.Streitmatter, J.W.Mitchell, L.M.Ba r bier USRA: A. A.Moissev, J.F.KrizmanicLouisiana State University: G.Case, M. L. Cherry, T. G. Guzik, J. B. Isbert, J. P. WefelWashington University in St Louis: W. R. Binns, M. H. Israel, H. S. KrawzczynskiUniversity of Denver : J. F. Ormes
Italy : 3 organizations 16 membersUniversity of Siena and INFN: P.S.Marrocchesi , A.Cardarone, R.Cessi, M.G.Bagliesi, G.Bigongiari , P.Maestro, V.Millucci , R.Zei University of Florence and INFN: O. Adriani, P. Papini, L. Bonechi, L.E. VannucciniUniversity of Pisa and INFN : C.Avanzini, M.Y.Kim, T.Lomtadze, F.Morsani
China : 2 organizations 6 membersPurple Mountain Observatory, Chinese Academy of Science: J. Chang, W. Gan, T. LuInstitute of High Energy Physics, Chinese Academy of Sciences: Y.Ma, H.Wang, G.Chen
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CALET:CALorimetric Electron Telescope
CALET Objectives Cosmic Ray Origin and Propagation Gamma-ray Sources Dark Matter Gamma-ray Bursts Solar Physics
Dark Matter
AGN Pulsar
SNR
Japanese Experiment Module (Kibo)
International Space Station
CALET
Cosmic Rays & Gamma Rays
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CALET OverviewCALET Overview
CALET Mission Concept
Observation: Electrons in 1GeV - 10 TeV Gamma-rays in 20 MeV - * TeV + Gamma-ray Bursts in 7 keV - 20MeV P-Fe in several 10GeV - 1000 TeV
Launch: HTV: H-IIA Transfer Vehicle
Attach Point on the ISS: Exposed Facility of Japanese Experiment Module (JEM-EF)
Life Time: 3(min.) - 5 years
Mission Status Phase A/B Study Launch around 2013 in Plan
CALET Payload High Energy Electron and Gamma- Ray Telescope Consisted of - Imaging Calorimeter - Total Absorption Calorimeter Weight: 1500 kg Geometrical Factor: ~0.7 m2sr Power Consumption: 640 W Data Rate: 300 kbps
JEM/EF
CALET
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Purposes of Electron Observation
Expected Electron Spectrum by the CALET Observation for 3 years(~ 1000 m2 sr day)
Cygnus Loop20,000 years2,500 ly
Monogem86,000 years1,000 ly
Vela 10,000 years820 ly
Chandra
ROSAT
・CALET
Vela
近傍ソースの検出-エネルギースペクトル-到来方向の異方性
超新星における衝撃波加速加速機構と拡散過程超新星の頻度、分布
太陽変調
Anisotropy
W=1048 erg/SNI(E)=I0E-α
N =1/30yrD=D0(E/TeV)0.3
Search for the signature of nearby HE electron sources (believed to be SNR) in the electron spectrum above ~ TeV
Search for anisotropy in HE electron flux as an effect of the nearby sources.
Precise measurement of electron spectrum above 10 GeV to define a model of accele-ration and propagation.
Observation of electron spectrum in 1~10 GeV for study of solar modulation
Possible Nearby Sources• T< 105 years• L< 1 kpc
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Positron will be measured by - PAMELA flying- AMS to be launched on ISS- CALET on ISS ( can not separate e+ and e-) Simulation for 300 GeV KK DM
Dark Matter Search by Positrons ( & Electrons )Dark Matter Search by Positrons ( & Electrons )
H.C. Cheng et al., PRL 2002.
Direct decay to e+ e-
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Gamma-Ray Observation in 20 MeV~several TeVGamma-Ray Observation in 20 MeV~several TeVCALET on the ISS orbit without attitude control of the instrument: Wide FOV ( ~45o ) and Large Effective Area (~0.5 m2 ) in 20 MeV- 10 GeV ⇒
Excellent Energy Resolution ( < a few %) over 100 GeV ⇒
Sky coverage of 70 % for one day All sky coverage in 20 days Typical exposure factor of ~50 days in one year for point source
Measurement of change of power-law spectral index Possible detection of line gamma-rays from Neutralino annihilation
Energy Resolution
better than GLAST over 10 GeV
SΩ~5000cm2sr
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Neutralino annihilating to γγ Maximal annihilation rate of σ v in L.Bergstorm et al. PRD (2001)
SUSY Dark Matter Search by Gamma-ray LineSUSY Dark Matter Search by Gamma-ray Line WIMP Mass Limit from Direct Observation WIMP mass is likely heavier than ~100 GeV Future accelerator experiments will cover the mass range in 100~1000 GeV Indirect observation is very promising to see gamma-ray line according to WIMP mass.
Expected line signal for 3 year observation
CALET Observation of SUSY Dark Matter
Gamma-ray linesensitivity toward the Galactic center(300 〇 <l<60 〇 , |b|<10 〇
), compared to the gamma-ray line flux from Nutralino annihilation.
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Origin and Propagation of Proton and NucleusOrigin and Propagation of Proton and Nucleus- Supernova Shock Acceleration- Supernova Shock Acceleration Change of power spectrum index depending on Z ?Change of power spectrum index depending on Z ?-- Propagation in the Galaxy Propagation in the Galaxy Leaky box model ?Leaky box model ?
Measurements of proton and heavy ion flux in the energy region exceeding 1 TeV, in which magnet spectrometer is not capable.
Energy (TeV) Number
1 ~106
10 2.3 × 104 100 4.1 × 102
1000 ~10
For proton measurement: SΩeff ~ 0.2 m 2 sr (for p) Exposure factor for 3 years: 220 m 2 sr day~ 1.9× 10 7 m 2 sr sec Expected numbers of protons:
Energy Resolution: ~30% , E > 100 GeV
P & HeHeavy Nuclei
B/C Ratio
Conceptual Structure of CALETConceptual Structure of CALET
Requirements: Large Acceptance and Long Exposure: ~1000 m2 sr day Shower Imaging Capability: < 1mm Hadron Rejection Power: > 105
Energy Measurement: 20 MeV~10 TeV for e, several 10 GeV ~ 1000 TeV for hadrons
Detector Weight: 1450 kgTotal Absorber Thickness: 32 r.l, ~1.7m.f.p
Schematic Side View of CALET
SciFi/W Imaging Calorimeter (IMC): Area: ~ 0.8 m2
SciFi Belt: 1mm square x ~1 m length 17 layers (x &y) Tungsten Thickness : 4 r.l , 0.15 m.f.p
Total Absorption Calorimeter (TASC): Area: ~0.36 m2
BGO Log: 25 x 25 x 300 mm 6 layers (x & y) Thickness: 28 r.l , 1. 5 m.f.p
・ Anti-Coincidence Detector for Low E. γ ・ Silicon Array for High Z and Particle ID
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Examples of Simulation EventsExamples of Simulation Events
Shower Profiles by SimulationShower Profiles by SimulationGamma-ray 20 MeV
Gamma-ray 100MeV
Gamma-ray 1GeV
Gamma-ray 10GeV
Electron 10 GeV
Electron 100 GeV
Electron 10 TeV
Proton 3 TeV
Proton 3 TeV
pair creation
pair creation
shower
shower
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シリコンアレイ(SIA)
イメージングカロリーメータ
(IMC)
トータルアブソープションカロリーメータ
(TASC)
アンチコインシデンスディテクタ
(ACD))
SIA
IMC
TASC
ACD
Schematic Structure of the CALET PayloadSchematic Structure of the CALET Payload
GBM
MDP
VSC
GBM: Gamma-Ray Burst MonitorVSC: Visual Sky SensorMDP: Mission Data Processor
ACD:Anti-coincidence DetectorSIA: Silicon Pixel ArrayIMC: Imaging CalorimeterTASC: Total Absorption Calorimeter
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Scintillating Fibers(64 fibers = 1 unit)
Tungsten Prate+
Honeycomb Plate
Side Support Structure
1 Layer
Front End Processor Units
FEC +64 anode PMT
ATCS Coldplate
Scintillating Fibers(64 fibers = 1 unit)
Tungsten Prate+
Honeycomb Plate
Side Support Structure
1 Layer
Front End Processor Units
FEC +64 anode PMT
ATCS Coldplate
BGO(12 x6 x2)FEC
SUPPORT PANELS
CFRP BGO CASE
PDPMT
BGO(12 x6 x2)FEC
SUPPORT PANELS
CFRP BGO CASE
PDPMT
Details of Each ComponentDetails of Each Component
(by NASA/Goddard)
IMC: Imaging Calorimeter TASC: Total Absorption Calorimeter
SIA: Silicon Pixel Array ACD: Anti-Coincidence Detector
One pixel: 11.25 mm x 11.25 mmx 0.5 mm 6400 pixels array x 2 layers Charge resolution: 0.1e for p, 0.35e for Fe( by Siena U. and Florence U.) Segmented Plastic Scintillators
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Detector DevelopmentDetector DevelopmentSciFi Belt 64-anode PMT
FEC ( VA32, TA, 16bits ADC, FPGA)
BGO
Si PIN Photodiodes FEC with PD
BGO
SciFi Belt
PMT
FECBGO
FEC
PD
-
-
-
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Gamma-Gamma- rr ay Burst Monitoray Burst Monitor
Energy Range: 7keV- 20 MeV
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CALET launched by CALET launched by HTVHTV
CALET
HTV
HTV
ISS
Approach to Approach to ISSISS
Pickup of Pickup of CALETCALET
H-IIA Transfer VehicleH-IIA Transfer Vehicle (( HTV)HTV)
Launching of H-II RocketLaunching of H-II Rocket Separation from H-IISeparation from H-II
Launching Procedure of CALET
CALET
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CALET TimelineCALET Timeline
2009 2010 20112006
JEM-EF Utilization
2013201220082007JFY 2009 2010 20112006
JEM-EF Utilization
2013201220082007JFY
ProposalAO
Selection(3 missions)
Selection for Development Phase(Concentrate to one mission)
Dev
elop
men
tP
hase
Def
initi
on
CALETLaunch
Conceptual Design PreliminaryDesign
CriticalDesign
MaintenanceDesign &
FM IntegrationMission Definition
SDR
Phase A/B Phase C/D
Development PhaseDefinition Phase
BBMEM/PM
FM (Int’l Partners’ Components)
PFM/FM (system level)
1st round Utilization
2nd round Utilization
SEDA, MAXI(J) SMILES(J)RAID/HICO(US)
2J/A HTV#1 HTV#2 HTV#3 HTV#4 HTV#5TBD TBD TBD (CALET)
(Review of progress)
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We have successfully been developing the CALET instrument for JEM/EF facility from the experience of balloon experiments.
The CALET has capabilities to observe the electrons up to 10 TeV , gamma-rays in 20 MeV- several TeV , proton and heavy ions in several 10 GeV - 1000 TeV, for investigation of high energy phenomena in the Universe.
We have already completed a pre-phase A study within last 6 years*. JAXA has selected CALET as one of three mission candidates in May,
2007 for concept study and definition of mission instrument
(~Phase A/B) . CALET will be launched around 2013 if it will be approved by the next s
election expected after two years. *)This work is supported by a part of “Ground-based Research Announcement for Sp
ace Utilization” promoted by Japan Space Forum
Summary and Future ProspectSummary and Future Prospect
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Characteristics of Cosmic-Ray Electrons Electron Energy Loss by - Inverse Compton Scattering - Synchrotron Radiation
Electron Propagation in the Galaxy - Diffusion Process
Energy Loss Rate dE/dt = bE2
T(Age ) = 1/bE
R(Distance)=(2DT)½
1 TeV Electron Source: Age < 105 years Distance < 1 kpcVelaCygnus LoopMonogem orUnobserved Sources?
Ec=∞Ec=20TeVEc=10TeV
max min
max min
3 3
2i i
iii
I I D N R
I I c N ct
2( ) ( )dNe
D Ne bE Ne Qdt E
Electron Density Equation
Anisotropy
Nearby Source Candidates
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Model Dependence of Nearby Source Effect
Ec=∞ 、 ΔT=0 yr, Do=2x1029 cm2/s Do=5 x 1029 cm2/s
Ec= 20 TeV Ec=20 TeV 、 ΔT=1-104 yr
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Cosmic-Ray Electron Energy Spectrum
PPB- BETS
The number of electron candidates = 84 events
ECCATICBETS
PPB- BETS
The number of electron candidates = 84 events
ECCATICBETS
ECCATICBETS
PPB-BETS
The number of electron candidates = 84 events
ECCATICBETS
E3 ×J Spectrum
New Sources ?
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JEM (KIBO) PM & EF
JEM PM (Pressurized Module)
GPS AntennaJEM ELM-PS (Experiment Logistics Module Pressurized Section)
JEMRMS Main Arm
JEMRMS SFA(Small Fine Arm)Air Lock
HTV Antenna
JEM EF(Exposed Facility) ICS
(Inter-OrbitCommunication System)
JEM ELM-ES (Experiment Logistics Module Exposed Section)
JEM will be completed in 2009
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Institution Current Project Contribution in CALET Co PI
NASA/Goddard GLAST, BESS Anti-coincidence Detector R. E. Streitmatter w/ U. of Denver Simulations J. F. Ormes
Washington U. ACE, TIGER Scintillating Fiber Detector W. R. Binns S/C – ISS interface unit
Louisiana State U. ATIC BGO Calorimeter* J. P. Wefel
U. of Siena and Pisa AMS,CREAM Silicon Detector P. S. Marrocchesi
U. of Florence PAMELA DAQ System, Silicon Detector O. Adriani
Purple Mountain Obs. Lunar Mission BGO Calorimeter, Simulation J. Chang
International Collaboration Team
*Detector components in support of TASC development.
Tentative assignments: Final decisions to be made during Phase A/B.