ＣＡＬＥＴプロジェクト：
国際宇宙ステーション日本実験棟（きぼう）における宇宙科学観測ミッション
CALET Project:
Astrophysics Mission for Japanese Experiment Module(Kibo) at the ISS
CALET
CALET

Shoji Torii

on behalf of the CALET Collaboration
Waseda University& JAXA/Space Environment Utilization Center
April 27, 20102011.08.31

RIKEN Workshop

宇宙線研究所セミナー

1

CALET International Collaboration TeamJAPAN

Waseda University
JAXA/Space Environment Utilization Center
JAXA/ Institute of Aerospace and Astronautical Sciences
Kanagawa University,
Aoyama Gakuin University
Shibaura Institute of Technology
Institute for Cosmic Ray Research , University of Tokyo
Yokohama National University
Hirosaki University
Tokyo Technology Inst.
National Inst. of Radiological Sciences
High Energy Accelerator Research Organization (KEK)
Kanagawa University of Human Services
Saitama University
Shinshu University
Nihon University
Ritsumeikan University

Funding Agencies
JAXA/SEUC

Waseda University
supported also by
JSPS, MEXT

USA

NASA

ITALY

ASI

NASA/GSFC
Louisiana State University
Washington University in St Louis
University of Denver
University of Siena
University of Florence & IFAC (CNR)
University of Pisa
University of Roma Tor Vergata

CALET Collaboration Member
O. Adriani19 , K.Asano17, M.G. Bagliesi22, G. Bigongiari22, W.R. Binns24, S. Bottai19, J.Buckley24,
G. Castellini19, M.L. Cherry9, G. Collazuol20, K. Ebisawa5, V. Di Felice21 , H. Fuke5, T.G. Guzik9,
T. Hams 10 , N. Hasebe 23 , M. Hareyama 5 , K. Hibino 7 , M. Ichimura2 , K. Ioka 8, J. B. Isbert 9 ,M. H. Israel24, E. Kamioka15, K. Kasahara23, Y. Katayose25, J. Kataoka23, R.Kataoka17, N. Kawanaka8,
M.Y. Kim22, H. Kitamura11, Y. Komori6, T. Kotani23, H.S. Krawzczynski24, J.F. Krizmanic10, A. Kubota15,
S. Kuramata 2 , T.Lomtadze 20 , P. Maestro 22 , L. Marcelli 21 , P. S. Marrocchesi 22 , V. Millucci 22 ,J.W. Mitchell10, K. Mizutani14, A.A. Moiseev10, K.Mori23, M. Mori13, F. Morsani20, K. Munakata16,
H. Murakami23, Y.E.Nakagawa23 , J. Nishimura5, S. Okuno7, J.F. Ormes18, S. Ozawa23, P. Papini19,
B.Rauch 24 , S.Ricciarini 19 , Y. Saito 5 , M. Sasaki 10 , M. Shibata 25 , Y. Shimizu 4 , A. Shiomi 12 ,R. Sparvoli 21 , P. Spillantini 19 , M. Takayanagi 5 , M. Takita 3 , T. Tamura 7 , N. Tateyama 7 ,T. Terasawa3, H. Tomida5, S. Torii23, Y. Tunesada17, Y. Uchihori11, S. Ueno 5, E. Vannuccini19,
J.P. Wefel9, K.Yamaoka1, A. Yoshida1, K. Yoshida15, T. Yuda3
1) Aoyama Gakuin University, Japan
2) Hirosaki University, Japan
3) ICRR, University of Tokyo, Japan
4) JAXA/SEUC, Japan
5) JAXA/ISAS, Japan
6) Kanagawa University of Human Services, Japan
7) Kanagawa University, Japan
8) KEK, Japan
9) Louisiana State University, USA
10) NASA/GSFC, USA
11) National Inst. of Radiological Sciences, Japan
12) Nihon University, Japan
13) Ritsumeikan University, Japan

14) Saitama University, Japan
15) Shibaura Institute of Technology, Japan16) Shinshu University, Japan17) Tokyo Technology Inst., Japan
18) University of Denver, USA19）University of Florence and IFAC(CNR), Italy20) University of Pisa, Italy21) University of Rome Tor Vergata , Italy
22) University of Siena, Italy
23) Waseda University, Japan
24) Washington University - St Louis, USA
25) Yokohama National University, Japan

CALETの経緯

CALET Observation
Calorimeter (CALET/CAL)• Electrons: 1 GeV – 20,000 GeV• Gamma-rays: 10 GeV – 10,000 GeV(Gamma-ray Bursts: > 1 GeV)
• Protons and Heavy Ions:
several tens of GeV – 1,000 TeV• Ultra Heavy Ions：
over the rigidity cut-off

Gamma-ray Burst Monitor (CGBM)• Soft Gamma-rays : 30 keV – 30 MeV• Hard X-rays: 3keV – 3 MeV
Science Objectives
Nearby Cosmic-ray Sources
Dark Matter

A Detector Dedicated to Electron
Observation in 1GeV-20,000GeV

Observation Targets
Electron spectrum in trans-TeV region
Signatures in electron/gamma energy spectra in 10
GeV – 10 TeV region

Origin and Acceleration of Cosmic Rays

p-Fe over several tens of GeV, Ultra Heavy Ions

Cosmic –ray Propagation in the Galaxy

B/C ratio up to several TeV /nSolar Physics

Electron flux below 10 GeV

Gamma-ray Transients

Gamma-rays and X-rays in 3 keV – 30 MeV

CALET Payload
Items
MissionEquipment

Specification
CAL: Calorimeter
CGBM: Gamma-ray Burst Monitor

LaunchCarrier

HTV-5

LaunchTargetDate

JFY 2013 (TBD)

Mission
PeriodMore than 2 years (5 years target)

Mass

586 kg (Nominal) ― 620kg (Max)

Envelope

Standard Payload SizePower

Less than 500 W

Data Rate

Medium Data Rate : 300 kbps
Low Data Rate : 20 kbps

CALET Detector System

Support Sensor

JEM/EF Equipment

Calorimeter: CHD,IMC, TASC+MDC
GBM : HXM, SGM

GPSR
ASC

FRGF

Electron and Positron Observation
Cosmic-ray Energy SpectraCosmic-ray
protons

Spectrum of electrons: softer than protons
 power-law index:
e:~-3.0, p:-2.7
Cosmic-ray
electronsa few electrons/ cm2 sr day

Flux of electrons and positrons:~1 % of protons @10GeV~0.1 % @ 1000GeV~0.1 % @ 10 GeV

a few electrons/ m2 sr day=> As higher energies,

Lower electron flux
Lager proton backgrounds

Large amount of exposureswith a detector of high proton rejection power (+ charge separation)Long duration balloon flight in 10~1000 GeV (~10 m2srday)
Observation in space for years over 1000 GeV (> 100 m2srday)
April 27, 2010

RIKEN Workshop

7

e± Propagation∂∂bε e2 f  + q t , ε e , x
f t , ε e , x= D ( ε e ) ∇ 2 f +
∂t
∂ε e

(

)

(

Diffusion

Energy loss by
IC & synchro.

b ~ 10−16 GeV -1s −1εe D ( ε e ) ~ 5.8 ×10 cm s 1 +

4GeV



)

Injection

13

28

2 −1

← B/C ratio−αe

For a single burst with q ∝ ε Power law spectrum
q0ε e−αα − 2 −( d d )1 − btε e ) ef
1
32 3 (
π d diff2

diff

d diff ( t , ε e ) ~ 2  D ( ε e ) t 

April 27, 201012
Atoyan 95, Shen 70
Kobayashi 03

RIKEN Workshop

εcut ~

bt
8

Electron & Positron Observation
Astrophysical Origin

Production Spectrum
Acceleration in PWN

Log(dN/dE)

Shock Wave Acceleration in SNR（Power Law Distribution ＋Cutoff）
dN/dE ∝ E-2exp(-E/Ec)

Propagation in the Galaxy• Diffusion Process• Energy Loss
dE/dt =-bE2（Syncrotron＋Inverse Compton）• π+/- or K+/- → µ+/- → e+/-

⇒

⇒
↑
Ec

e++e-

⇒

Log(E)

Evolution of the Universe

Dark Matter Origin
Constitutes of
宇宙の質量構成比
the Universe

暗黒エネルギー
暗黒エネルギー 暗黒物質
暗黒物質

重元素Element
Heavy
重元素
0.03%
0.03%
ニュートリノNeutrino
0.3%
ニュートリノ
0.3%
星
Star
0.５%
%
星 0.5
0.５%
Hydrogen、水素、ヘリウム
Helium
水素、
４%
ヘリウム
４%
暗黒物質
Dark
Matter
暗黒物質
25%
2３%
25%
暗黒エネルギー
Dark
Energy70%
7３%

July 21, 2010⇒MχAnnihilation of Dark Matter（WIMP)
χχ→e+,e-COSPAR

Production Spectrum(ⅰ) Monoenergetic: Direct Production of e+e- pair（ⅱ） Uniform：Production via Intermediate Particles（ⅲ） Double Peak： Production by Dipole Distribution
via Intermediate Particles

9

A Naïve Result from Propagation
T (age) = 2.5 X 105 X (1 TeV/E) yr

1 GeV Electrons

GALPROP/Credit S.Swordy

R (distance) = 600 X (1 TeV/E)1/2 pc

1 TeV Electron Source: Age < a few105 years
very young comparing
to ~107 year at low energies

 Distance < 1 kpc
nearby source

Source (SNR) Candidates :Vela

Cygnus Loop Monogem

Unobserved Sources?
April 27, 2010

100 TeV Electrons(F0: E3 x Flux at 3TeV)

Model Dependence of Energy Spectrum and 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

April 27, 2010

RIKEN Workshop

Kobayashi et al. ApJ (2004)
11

New Calculation for SNR Origin
S.Profumo arXiv:0812.4457v2 28 Apr. 2009

Source Candidates

Positron Ratio
April 27, 2010

Electron + Positron

RIKEN Workshop

12

Observed (e++e-)Spectra (as of 2008) & e+/(e++e-) Ratio
J. Chang et al. Nature (2008)

PAMELA e+/(e++e-) Ratio (RICAP, 2009)
statistics improved by ~2.5 ÷ 3

AMS (stars) HEAT (triangles)
BETS (circles) PPB-BETS (crosses)
Emulsions (diamonds) ATIC (red circles)• If we assume the power law spectrum

NatureMLP+BDTD(+data, no pre-sampler,
improved knowledge of detectors)• The positron ratio observed by PAMELA
presents unexpected increase over 10 GeV.

( with γ=-3.3) calculated by GALPROP,an excess of (e++e-) is seen in 300-800 GeV. • This increase can be understood if

the positrons are created by Nearby Pulsars• The excess might be contributed fromexotic sources: Nearby Pulsars or WIMPs. or WIMPs in addition to secondary process.

April 27, 2010

Both anomalies from same reason ?
To identify the reason, Anisotropy in (e++e-) ande+/(e++e-) over 100 GeV are indispensable.

13

ICRC2011

Extending the Positron to Electron Fraction
PAMELA NEW RESULTS?

TMVA analysis for data with E>15 GeV

ICRC2011

Geomagnetic field + Earth shadow = directions fromwhich only electrons or only positrons are allowed

events arriving from West:e+ allowed, e- blocked

events arriving from East:e- allowed, e+ blocked
For some directions, e- or e+ forbidden
Pure e+ region looking West and pure e- region looking East
Regions vary with particle energy and spacecraft position
To determine regions, use code by Don Smart and Peggy Shea (numericallytraces trajectory in geomagnetic field)• Using International Geomagnetic Reference Field for the 2010 epoch••••

ICRC 2011, Beijing

Justin Vandenbroucke: Fermi LAT positron
spectrum

15

ICRC2011

Final results: positron fraction• Fraction = ϕ(e+) / [ϕ(e+) + ϕ(e-)]• We don’t use the both-allowed region except as a cross check• Positron fraction increases with energy from 20 to 200 GeV
ICRC 2011, Beijing

Justin Vandenbroucke: Fermi LAT positron
spectrum

16

Then, excellent observations of (e++e-) in statistics are carriedout by FERMI-LAT and HESS, and a new era of electron
observation is opened probably by indicating a flattening ofenergy spectrum and a sharp cut-off over 1 TeV, respectively.
F.Aharanian et al. arXiv:0905:0105

I really appreciate their efforts to derive the electron spectrumin unexploded region.
April 27, 2010
RIKEN Workshop

17

ICRC2011

Currently available results on high energy CRE

Fermi LAT results:• PRL 102, 181101, 2009 reported the spectrum from 20 GeV to 1 TeV, taken in the first 6 monthsof operation. Total statistics 4.7M events. Most cited Fermi LAT paper so far (over 450 times)• PRD 82, 092004, 2010: spectrum from 7 GeV to 1 TeV, collected in the 1st year. Total statistics
7.95 M events. More than 1000 events in highest energy bin (772 – 1000 GeV)
Alexander Moiseev
32th ICRC
August 11, 201118

PAMELA electron (e-) spectrum

ICRC2011

Adriani et al., Phys. Rev. Lett. 106, 201101 (2011), arXiv: 1103.2880~3% syse-e+ + e-~7% sysElectron Observation for Nearby Sources
Expected Anisotropy
from Vela SNR~10% @1TeV

Expected Flux
> 1000827

644

Monogem
April 27, 2010

Cygnus LoopVela

RIKEN Workshop

20

ICRC2011

CR Electrons Anisotropy

No-anisotropy map

Ackermann et al., Fermi LAT
Collaboration, Phys Rev D82, 092003,2009

 Search for CR electrons anisotropy provides an information on:• Local CR sources and their distribution in space• propagation environment• heliospheric effects• presence of dark matter clumps producing e+ e-

Flight data sky map

 Result:• More than 1.6 million electron events with energy above 60
GeV have been analyzed on anisotropy• Upper limit for the dipole anisotropy has been set to 0.5 –
5% (depending on the energy)

Significance map•Upper limit on fractional
anisotropic excess ranges
from a fraction to about one
percent (depending on theminimum energy and theanisotropy’s angular scale)
Dipole anisotropy vs. minimum energy. Solid• Our upper limits lie
line: Galprop spectrum, dashed line –roughly on or above theMonogem, dotted line – Vela
Alexander
Moiseev
32th ICRC
predicted
anisotropies
21
August 11, 2011

Circles: Fermi LAT 95 % CL dataElectron (+ Positron) from Dark Matter Annihilation
Chang et al. (2008)

Expected energy spectrum
from Kaluza-Klein Dark Matter(m=620GeV)

Boost Factor ~200

Expected e-+e+ energy spectrum by
CALET in case of the ATIC observation
2 years （BF=40)
or 5 years（BF=16)

Dark Matter detection
capability by CALET
22

Electron and Positron from Dark Matter Decay
Decay Mode: D.M. -> l+l-ν
Mass: MD.M.=2.5TeV
Decay Time: τD.M. = 2.1x1026 s

Expected e-+e+ energy spectrumby CALET observation

Expected e+/(e-+e+) ratio by atheory and the observed data

Observation in the trans-TeV region
Dark Matter signal
Ibarra et al. (2010)23

Electron Observation (5 years) – Astrophysical ModelKK DM(Δt=0) vs SNR type (Δt=105 year)

CALET Observation

CALET Observatuib----- KK DM----- Pulsar TypeSNR Type

SNR Type

SourceSNR Type（exp(-t)）

age=5.6x105 yr,

Q0 (t ) ∝Ee=1.7x1050 erg,

SNR Type vs Pulsar (Δt=3×105 year)

Etot ln 4

τ0 t ln 4 exp −
τ0 
Pulsar Type（ｔ-2)
Q0 (t ) ∝ Lspindown =Etot
τ 0 (1 + t / τ 0 )2

spectral index=1.7
τ0τ0April 27, 2010

RIKEN Workshop

24Diffuse Gamma-Ray Observation

Electron origin

Simulated CALET gamma-ray all sky map
for 3yr (>10GeV)
Vela pulsar

proton origin

Detection limit of Galactic
diffuse gamma rays

CALET

Extra-galactic diffuse
gamma-ray spectra

GemingapulsarExtragalactic Diffuse Gamma-rays from Dark
Matter Decay
Decay Mode: D.M. -> l+l-ν
Mass: MD.M.=2.5TeV
Decay Time: τD.M. = 2.1x1026 s

EGRET

Extra-galactic diffuse
gamma-rays
Extragalactic background+Gamma-rays from inverse
Compton scattering of theelectrons and positrons from DM
decay with the inter-stellar andextragalactic photons+
Gamma-rays from DM

Observation in the sub-TeV
regionDark Matter signal
Ibarra et al. (2010)26

Gamma-ray line from Dark Matter
WIMP Dark Matter （Neutralino, Kaluza-Klein D.M.）
Annihilation or Decay
Gamma-ray Line2yr （BF=5)or 5yr （BF=2)

Excellent energy resolution with CALET（2%：10GeV〜10TeV）
Detection for gamma-ray line due
to DM annihilation or decay

Expected gamma-ray line for
DM (m=830 GeV) annihilation
by CALET observation(ref. Bergstrom et al. 2001)

Proton and Nucleus Observation （5years)
2ry/ 1ry ratio ( B/C)
 Energy dependence of diffusion constant: D ~ Eδ Observation free from the atmospheric effect up
to several TeV/n

C

O

Ne

Mg

Si
April 27, 2010

CREAM

Leaky Box Model
Nearby Source Model (Sakar et al.)Fe
RIKEN Workshop

28

ICRC2011

CREAM Results showing hardening of spectra around 200 GeV/nICRC2011

PAMELA proton and alpha spectra
Science 332 (6025): 69-72 (2011)
protonsalphas• ~E-2.7 power law• Proton flux an order of magnitude larger than alpha flux
ICRC 2011, Beijing

Justin Vandenbroucke: Fermi LAT positron
spectrum

30

ICRC2011

TRACER

B/C ration up to 1TeV/nCREAM

CALET System Configuration

Total Mass of Payload : 586 kg (Nominal) ― 620kg (Max) Detector: Calorimeter, Gamma-ray Burst Monitor (HXM, SGM) + MDC
 Support Sensor: Advanced Sky Camera, GPS Additional Sensor: Compact Infrared Camera for Earth Observation (CIRC)(IA)CALET/CAL Instrument
450 mmExpected Performance( from Simulations and/or Beam Tests)• SΩ：1200 cm2sr for electrons
1000 cm2sr for gamma-rays• ΔE/E :a few % (>10 GeV) for e,γ’s~30 % for protons• e/p separation : 10-5
• Charge resolution : 0.15-0.3 e• Angular resolution : Preliminary
0.24-0.76 deg. for gamma-rays
Shower particles

CHD(Charge Detector)

IMC(Imaging Calorimeter)

TASC(Total Absorption Calorimeter)

Function

Charge Measurement (Z=1-40)

Arrival Direction, Particle ID

Energy Measurement, Particle ID

Sensor(+ Absorber)

Plastic Scintillator : 14 × 1 layer (x,y)
Unit Size: 32mm x10mmx450mm

SciFi : 448 x 8 layers (x,y) = 7168
Unit size: 1mmsq x 448 mm
Total thickness of Tungsten: 3 r.l.

PWO log: 16 x 6 layers (x,y)= 192
Unit size: 19mm x 20mm x 326mm
Total Thickness of PWO: 27 r. l.

Readout

PMT+CSA

64 -anode PMT+ ASIC

APD/PD+CSA
PMT+CSA ( for Trigger)

CALET Shower Imaging Capability (Simulation)
Gamma-ray 10 GeV

Electron 1 TeV

Proton 10 TeV

In Detector Space

Proton rejection power of 105 can be achieved with the IMC and TASC shower
imaging capability.
Charge of incident particle is determined to ΔZ=0.15-0.3 with the CHD.

CALET Prototype Test
Balloon Experiment of the CALET Prototype (1/4 - Scale of CALET) in 2009 , bCALET2
bCALET2 Detector

Schematic Side View
Example of Observed Electron Candidate

Experimental results of energy deposit by
10 GeV e, compared with GEANT4 and EPICS

CERN-SPS Beam Test of the Scale-modelof CALET in 2009, 2010 (2011)
Configuration of Detector

Development of Bread Board Model
IMC
SciFi Layer

TASC
PWO + APD/PD

CHD
Plastic Scintillator+ Light Guide

Structure of IMC

Structure of TASC

Design Study of Structure

Random Vibration Test

Random Vibration Test

3.1 CGBM instrumentation – Sensors – 2 Hard X-ray Monitors (HXMs)

HXM• LaBr3(Ce) (φ66 mm x 0.5 inch)with a 410um thick beryllium
window by Saint Gobain Crystals.
This crystal is used in GRB
observations for the first time.
• Hamamatsu 2.2-inch
PMT R6232-05• High voltage divider and charge-sensitive amplifier

Soft Gamma-ray Monitor (SGM)• BGO (φ4 inch x 3 inch) + Light guide by OKEN Co Ltd.
• Hamamatsu 3-inch PMT R6233-20

SGM

2. GRB observations with CALET (I)• Simultaneous broadband coverage with CAL(GeV-TeV), CGBM(keVMeV), and possibly ASC (Advanced Star Camera: optical)• The CAL would be comparable to the CGRO/EGRET sensitivity.
Parameters

CAL

CGBM

Energy1 GeV- 10 TeV(GRB trigger)

HXM: 7keV– 1MeV (Goal 3 keV--3 MeV)
SGM: 100keV– 20MeV (Goal 30keV-30MeV)

Effective area

~1000 cm2

68 cm2 (2HXMs), 82 cm2 (SGM)

Angularresolution

2.5 deg@1 GeV,
0.4 deg@10 GeV

No localization capabilities by CGBM itself,
but IPN localization is possible

Field of view

~45 deg.(~2 str.)~π str. (HXM), ~4π str. (SGM)

Dead time~1.8 ms~20 usTime resolution

1 ms

GRB trigger：62.5 us (Event-by-event data)
Normal mode:1/8 s with 4 channels and 4 s
with 256 channels (Histogram data)

2. GRB observations with CALET (II)• Study of X-ray flashes (XRFs) and low energy portion of
normal GRBs with CGBM and MAXI/GSC (2—30 keV).
XRF
CGBM
MAXI

Normal GRB

HXM

SGM

7 keV – 20 MeV• Study of absorption featuresat 20-30 keV seen by Ginga/GBD.
• The CGBM effective area is comparable to that ofGinga/GBD (~60 cm2). We will expect to detect -40
GRBs/year by HXM and -80 GRBs/year by SGM.

at

CALET Performance for Electron Observation
Geometrical Factor (Blue Mark)

Detection Efficiency

SΩ ( for electrons) vs Incident Angle

Energy Resolution~2%

April 27, 2010

RIKEN Workshop

40

CALET Performance by Simulation

Efforts by the new experiments for deriving the positron andelectron spectra are really appreciated to open a door to new erain astroparticle physics.
We are waiting for much more study by ATIC, PAMELA, Fermi-LAT, HESS
and a forthcoming experiment in space, AMS-02.

Moreover,We need an accurate and very-high-statistics observation for searching Dark
Matter and/or Nearby Pulsars in the sub-TeV to the trans-TeV region with adetector which has following performance:
The systematic errors including GF is less than a few %.
The absolute energy resolution is as small as a few % ( ~ATIC).
The exposure factor is as large as more than 100 m2srday ( ~ FERMI-LAT).
The proton rejection power is comparable to 105 , and does not depend
largely on energies .

It should be a dedicated detector for electron observation in space.
Calorimetric Electron Telescope (CALET) is proposed.
42

Why we need CALET ?
CALET is a dedicated detector for electrons and has asuperior performance in the trans-TeV region as well asat the lower energies by using IMC and TASC

Proton rejection power depends fully on
simulation by using different parameters

104

FERMI Electron Analysis
Geometric Factor depends
strongly on energy

Energy resolution becomes worse
at high energies(~30 %@ 1 TeV)

Geometric
FactorResidual hadroncontamination

Expected CALET Performance
Geometric Factor is constant up to 10 TeV

Energy resolution is nearly 2 %,and constant over 10 GeVBlue Mark

Proton rejection power at 4 TeV
is better than 105 with 95 %electron retained
1.6 M protons

July 21, 2010COSPAR

43

Comparison of Detector Performance for Electrons
CALET is optimized for the electron observation in the tran-TeV region, and theperformance is best also in 10-1000 GeV.
Detector

EnergyRange(GeV)EnergyResolution

e/p SelectionPower

Key Instrument(Thickness of CAL)SΩT
（m２srday)

PPB-BETS(+BETS)

10 -1000

13%@100 GeV

4000(> 10 GeV)

IMC
(Lead: 9 X0 )~0.42

ATIC1+2(+ ATIC4)

10 a few 1000

<3%
( >100 GeV)

~10,000

Thick Seg. CAL(BGO: 22 X0)+ C Targets

3.08

PAMELA

1-700

5%@200 GeV

105

Magnet+IMC(W:16 X0)

~1.4
(2 years)

FERMI-LAT

20-1,000

5-20 %(20-1000
GeV)

103-104(20-1000GeV)

Tracker+ACD+ Thin Seg. CAL(W:1.5X0+CsI:8.6X0)

300@TeV(1 year)(less capability
in PM model)

1-1,000(Due toMagnet)～2.5％
＠100 GeV104(x 102 by TRD)

Magnet+IMC+TRD+RICH(Lead: 17Xo)~200(?)(5year)CALET

1-20,000~2%(>100 GeV)～105

IMC+Thick Seg. CAL(W: 3 Xo+ PWO : 27 Xo)

220(5 years)

AMS

Energy dep. GF

44

ICRC2011

TRD+ECAL: 0.09m2 sr

TRACKER: 0.4m2 sr => 0.09m2 sr(for current magnet)

Calorimeter Thickness: 17 X0=> Energy Leakage over 50 GeV

NIM 490 (2002) 132
April 27, 2010

RIKEN Workshop

46

Launching Procedure of CALET
CALET

H2B Transfer Vehicle（HTV)ISS

Pickup of CALET
HTV

HTV

Launching by
H2B Rocket

Approach toISS

Separation from H2B

CALET

Procedure of Payload Placement on JEM/EF Attach Point
Hand-off of HTV Palette

Pick up HTV PalettePlace JEM/EF Payload

CALET Attach Point in Japanese Experiment Module(Launching Schedule in 2013 by HTV5)

Concept of Data Downlink Stream

NASA Link
Real-Time Connection> 50 % (max. 17 hr/day)NASA Data
Archive Center

CALET

Waseda Univ.
CALET Mission
Science Center
JAXA ICS Link
Real-Time Connection~20 % (5 hr/day)International
Collaboration
Organization

Summary
CALET is a dedicated detector to electron observations in thetrans-TeV region, that will provide crucial information on
nearby sources and dark matter .
We have successfully developed the CALET instrument based onout experience of balloon-borne instruments (BETS, bCALET) andbeam tests of CALET proto-type detectors.
CALET has the capability to observe electrons up to 20 TeV ,gamma-rays from 10 GeV to 10TeV , protons and heavy ions fromseveral tens of GeV to ~1000 TeV, and ultra heavy ions to an
accuracy better than present balloon payloads.
The CALET project has been approved for launch with a schedulein 2013 (or 2014) JFY by HTV-5 to the Japanese Experiment
Module (Kibo). The project is currently in the final phase of“Preliminary Design Study” .