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

Sep. 14, 2007 TAUP07 2

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

Sep. 14, 2007 TAUP07 3

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

Sep. 14, 2007 TAUP07 4

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

Sep. 14, 2007 TAUP07 5

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

Sep. 14, 2007 TAUP07 6

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-

Sep. 14, 2007 TAUP07 7

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

Sep. 14, 2007 TAUP07 8

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.

Sep. 14, 2007 TAUP07 9

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

Sep. 14, 2007 TAUP07 11

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

Sep. 14, 2007 TAUP07 13

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

Sep. 14, 2007 TAUP07 14

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

Sep. 14, 2007 TAUP07 15

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

-

-

-

Sep. 14, 2007 TAUP07 16

Gamma-Gamma- ｒｒ ay Burst Monitoray Burst Monitor

Energy Range: 7keV- 20 MeV

Sep. 14, 2007 TAUP07 17

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

Sep. 14, 2007 TAUP07 18

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)

Sep. 14, 2007 TAUP07 19

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

Sep. 14, 2007 TAUP07 20

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

Sep. 14, 2007 TAUP07 21

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

Sep. 14, 2007 TAUP07 22

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 ?

Sep. 14, 2007 TAUP07 23

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

Sep. 14, 2007 TAUP07 24

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.