1. March 3, 2010 HEAD2010 1 Electron & Positron Observation Evolution of the Universe Dark Matter Origin ( ⅰ ) Monoenergetic: Direct Production of e+e- pair （ⅱ） Uniform ： Production via Intermediate Particles （ⅲ） Double Peak ： Production by Dipole Distribution via Intermediate Particles Production Spectrum ⇒ MχMχ Annihilation of Dark Matter （ WIMP) χχ→e +,e - Production Spectrum （ Power Law Distribution ＋ Cutoff ） Shock Wave Acceleration in SNR Acceleration in PWN Astrophysical Origin ⇒ dN/dE  E -2 exp(-E/E c ) Log(E) Log(dN/dE) EcEc ↑ Propagation in the Galaxy Diffusion Process Energy Loss dE/dt =-bE 2 （ Syncrotron ＋ Inverse Compton ） ⇒ ⇒  +/- or K+/-   +/-  e+/- e + +e -

2. March 3, 2010 HEAD2010 2 e ± Propagation For a single burst with Atoyan 95, Shen 70 Kobayashi 03 Power law spectrum Diffusion Energy loss by IC & synchro. Injection ← B/C ratio

3. (F 0 : E 3 x Flux at 3TeV) March 3, 2010HEAD20103 A Naïve Result from Propagation T (age) = 2.5 X 10 5 X (1 TeV/E) yr R (distance) = 600 X (1 TeV/E) 1/2 pc 1 TeV Electron Source: Age < a few10 5 years very young comparing to ~10 7 year at low energies Distance < 1 kpc nearby source Source (SNR) Candidates : Vela Cygnus Loop Monogem Unobserved Sources? 1 TeV Electron Source: Age < a few10 5 years very young comparing to ~10 7 year at low energies Distance < 1 kpc nearby source Source (SNR) Candidates : Vela Cygnus Loop Monogem Unobserved Sources? GALPROP/Credit S.Swordy 1 GeV Electrons 100 TeV Electrons

4. March 3, 2010 HEAD2010 4 Model Dependence of Energy Spectrum and Nearby Source Effect Ec=∞ 、 ΔT=0 yr, Do=2x10 29 cm 2 /s Do=5 x 10 29 cm 2 /s Ec= 20 TeV Ec=20 TeV 、 ΔT=1-10 4 yr Kobayashi et al. ApJ (2004)

5. March 3, 2010 HEAD2010 5 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 a detector 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 m 2 srday ( ~ FERMI-LAT). The proton rejection power is comparable to 10 5, and does not depend largely on energies. It should be a dedicated detector for electron observation in space. Calorimetric Electron Telescope (CALET) is proposed. Efforts by the new experiments for deriving the positron and electron spectra are really appreciated to open a door to new era in astroparticle physics.

6. March 3, 2010 HEAD2010 6 CALET Overview  Observation:  Electrons : 1-10,000 GeV  Gamma-rays : 10-10,000 GeV (GRB >100MeV) + Gamma-ray Bursts : 7 keV-20 MeV  Protons, Heavy Nuclei: several 10 GeV- 1000 TeV ( per particle)  Solar Particles and Modulated Particles in Solar System: 1-10 GeV (Electrons)  Instrument: High Energy Electron and Gamma- Ray Telescope Consisted of : - Imaging Calorimeter (Particle ID, Direction) Total Thickness of Tungsten (W) ： 3 X 0 Layer Number of Scifi Belts ： 8 Layers ×2(X,Y) - Total Absorption Calorimeter (Energy Measurement, Particle ID) PWO 20mm ｘ 20mm ｘ 320mm Total Depth of PWO ： 27 X 0 (24cm) - Silicon Pixel Array (Charge Measurement up in Z=1-35) Silicon Pixel 11.25mmx11.25mmx0.5mm 2 Layers with a coverage of 540x540 cm 2

7. March 2, 2010 HEAD2010 7 CALET Performance for Electron Observation SIA IMC TASC Electron 100 GeV Electron 1 TeV Geometrical Factor (Blue Mark) Detection Efficiency Energy Resolution ~2% See Poster for details ( Akaike et al.)

8. March 3, 2010 HEAD2010 8 The CALET mission instrument can satisfy the requirements as a standard payload in size, weight, power, telemetry etc. for launching by HTV and observation at JEM/EF. CALET System Design ＃９ Calorimeter Gamma-ray Burst MonitorStar Tracker Mission Data Controller Field of View (45 degrees from the zenith) JEM/EF & the CALET Port CALET Payload Weight : 483.5 kg Power Consumption: 313W

9. March 3, 2010 HEAD2010 9 CALET HTV ISS Approach to ISS Pickup of CALET H2-B Transfer Vehicle （ HTV) Launching of H-IIB Rocket Separation from H2-B Launching Procedure of CALET CALET

10. March 2, 2010 HEAD2010 10 Electron Observation (5 years) Vela Expected Anisotropy from Vela SNR Expected Flux > 1000 827 644 ~10% @1TeV Monogem Cygnus Loop

11. 11 Proton and Nucleus Observation （ 5years) O Mg Ne FeSi C CREAM 2ry/ 1ry ratio ( B/C)  Energy dependence of diffusion constant: D ~ E δ  Observation free from the atmospheric effect up to several TeV/n Nearby Source Model (Sakar et al.) Leaky Box Model

12. March 3, 2010 HEAD2010 12 Comparison of Detector Performance for Electrons Detector Energy Range (GeV) Energy Resolution e/p Selection Power Key Instrument (Thickness of CAL) SΩT （ m２srday) （ m ２ srday) PPB-BETS(+BETS) 10 -1000 13% @100 GeV 4000 (> 10 GeV) IMC : (Lead: 9 X 0 ) ~0.42 ATIC1+2 (+ ATIC4) 10 - a few 1000 <3% ( >100 GeV) ( >100 GeV)~10,000 Thick Seg. CAL (BGO: 22 X 0 ) + C Targets 3.08 PAMELA1-7005% @200 GeV 10 5 Magnet+IMC (W:16 X 0 ) ~1.4 (2 years) FERMI-LAT20-1,000 5-20 % (20-1000 GeV) 10 3 -10 4 (20-1000GeV) Energy dep. GF Tracker+ACD + Thin Seg. CAL (W:1.5X 0 +CsI:8.6X 0 ) 300@TeV (1 year) AMS1-1,000 (Due to Magnet) ～ 2.5 ％ ＠ 100 GeV 10 4 (x 10 2 by TRD ) Magnet+IMC+TRD+RICH (Lead: 17X o ) ~100(?)(1year) CALET1-10,000~2% (>100 GeV) ～ 10 5 IMC+Thick Seg. CAL (W: 3 X o + PWO : 27 X o ) 220 (5 years) CALET is optimized for the electron observation in the tran-TeV region, and the performance is best also in 10-1000 GeV.

13. March 3, 2010 HEAD2010 13 A New Technology and Space Experiments after CALET The Cosmic Ray Electron Synchrotron Telescope (CREST) (ICRC 2009, S.Nutter et al.) CREST payload for Ballooning: 40 days at 4 g/cm 2 in Antarctica Challenging New Technology: Synchrotron X rays from electron Expected electron detection efficiency  Very large acceptance: Vela detection up to 10 TeV (~ a few TeV for HESS )  High Threshold: E> 2 TeV  Poor energy resolution : ~ a factor of two 32x32 BaF 2 Crystals (40% coverage) 2.4 m E x > 30 keV TANSUO (J.Chang et al.) HEPCaT as part of OASIS (J.W. Mitchell et al.) Hodoscope + BGO Calorimeter SΩ~0.4 m 2 sr SΩ~2.5 m 2 sr Sampling Silicon-W Calorimeter + Secondary Neutron Detector

14. March 3, 2010 HEAD2010 14 The electron measurement over 1 TeV can bring us very important information of the origin and propagation of cosmic- rays and also of the dark matter ( yet not discussed here). We have successfully been developing the CALET instrument for Japanese Experiment Module (Kibo) – Exposed Facility to extend the electron observation to the tans-TeV region. The CALET has capabilities to observe the electrons up to 10 TeV, gamma-rays in 10GeV- 10TeV, proton and heavy ions in several 10 GeV - 1000 TeV, for investigation of high energy phenomena in the Universe. The CALET mission has been approved by the System Definition Review (SDR), and will proceed to the Phase B soon for launching in 2013. Summary and Future Prospect

15. March 3, 2010 HEAD2010 15 International Collaboration Team Waseda University: S. Torii, K.Kasahara, S.Ozawa, H.Murakami, Y.Akaike, T.Suzuki, R.Nakamura, K.Miyamoto, T.Aiba, M.Nakai, Y.Ueyama, N. Hasebe, J.Kataoka JAXA/ISAS: M.Takayanagi, H. Tomida, S. Ueno, J. Nishimura, Y. Saito H. Fuke, K.Ebisawa, M.Hareyama Kanagawa University: T. Tamura, N. Tateyama, K. Hibino, S.Okuno, T.Yuda Aoyama Gakuin University: A.Yoshida, T.Kobayashi, K.Yamaoka, T.Kotani Shibaura Institute of Technology: K. Yoshida, A.Kubota, E.Kamioka ICRR, University of Tokyo: Y.Shimizu, M.Takita Yokohama National University: Y.Katayose, M.Shibata Hirosaki University: S. Kuramata, M. Ichimura Tokyo Technology Inst.: T.Terasawa, Y. Tunesada National Inst. of Radiological Sciences: Y. Uchihori, H. Kitamura KEK: K.Ioka, N.Kawanaka Kanagawa University of Human Services: Y.Komori Saitama University: K.Mizutani Shinshu University: K.Munekata Nihon University: A.Shiomi Ritsumeikan University: M.Mori NASA/GSFC: J.W.Mitchell, A.J.Ericson, T.Hams, A. A.Moissev, J.F.Krizmanic, M.Sasaki Louisiana State University: M. L. Cherry, T. G. Guzik, J. P. Wefel Washington University in St Louis: W. R. Binns, M. H. Israel, H. S. Krawzczynski University of Denver: J.F.Ormes University of Siena: K. Batkov, M.G.Bagliesi, G.Bigongiari, A.Caldaroe, R.Cesshi, M.Y.Kim, P.Maestro, P.S.Marrocchesi, V.Millucci, R.Zei University of Florence and INFN: O. Adriani, L. Bonechi, P. Papini, E.Vannuccini University of Pisa and INFN: C.Avanzini, T.Lotadze, A.Messineo, F.Morsani Purple Mountain Observatory: J. Chang, W. Gan, J. Yang Institute of High Energy Physics: Y.Ma, H.Wang,G.Chen