1. Sep. 14, 2007TAUP071 The CALET Mission for Detection of Cosmic Ray Sources and Dark Matter Shoji Torii for the CALET Collaboration Research Institute for Science and Engineering Waseda University Sendai, Japan TAUP 07 Sep. 14th 2007

2. Sep. 14, 2007TAUP072 Member List (24 organizations, 74 members) Japan ： 14 organizations 38 members S. 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 members NASA/GSFC: R.E.Streitmatter, J.W.Mitchell, L.M.Ba ｒ bier USRA: A. A.Moissev, J.F.Krizmanic Louisiana State University: G.Case, M. L. Cherry, T. G. Guzik, J. B. Isbert, J. P. Wefel Washington University in St Louis: W. R. Binns, M. H. Israel, H. S. Krawzczynski University of Denver : J. F. Ormes Italy ： 3 organizations 16 members University 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. Vannuccini University of Pisa and INFN : C.Avanzini, M.Y.Kim, T.Lomtadze, F.Morsani China ： 2 organizations 6 members Purple Mountain Observatory, Chinese Academy of Science: J. Chang, W. Gan, T. Lu Institute of High Energy Physics, Chinese Academy of Sciences: Y.Ma, H.Wang, G.Chen

3. Sep. 14, 2007TAUP073 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

4. Sep. 14, 2007TAUP074 CALET 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 m 2 sr  Power Consumption: 640 W  Data Rate: 300 kbps JEM/EF CALET

5. Sep. 14, 2007TAUP075 Purposes of Electron Observation Expected Electron Spectrum by the CALET Observation for 3 years (~ 1000 m 2 sr day) Cygnus Loop 20,000 years 2,500 ly Monogem 86,000 years 1,000 ly Vela 10,000 years 820 ly Chandra ROSAT Anisotropy W=10 48 erg/SN I(E)=I 0 E -α Ｎ =1/30yr D=D 0 (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< 10 5 years L< 1 kpc

6. Sep. 14, 2007TAUP076 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 ) H.C. Cheng et al., PRL 2002. Direct decay to e + e -

7. Sep. 14, 2007TAUP077 Gamma-Ray Observation in 20 MeV~several TeV CALET on the ISS orbit without attitude control of the instrument: Wide FOV ( ~45 o ) and Large Effective Area (~0.5 m 2 ) 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~5000cm 2 sr

8. Sep. 14, 2007TAUP078 Neutralino annihilating to γγ Maximal annihilation rate of σ ｖ in L.Bergstorm et al. PRD (2001) SUSY 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 line sensitivity toward the Galactic center (300 〇 <l<60 〇, |b|<10 〇 ), compared to the gamma-ray line flux from Nutralino annihilation.

9. Sep. 14, 2007TAUP079 Origin and Propagation of Proton and Nucleus - Supernova Shock Acceleration Change of power spectrum index depending on Z ? Change of power spectrum index depending on Z ? - 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 ~10 6 10 2.3 × 10 4 100 4.1 × 10 2 1000 ~10 For proton measurement: SΩ eff ~ 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 & He Heavy Nuclei B/C Ratio

10. Conceptual Structure of CALET Requirements:  Large Acceptance and Long Exposure: ~1000 m 2 sr day  Shower Imaging Capability: < 1mm  Hadron Rejection Power: > 10 5  Energy Measurement: 20 MeV~10 TeV for e,   several 10 GeV ~ 1000 TeV for hadrons Detector Weight: 1450 kg Total Absorber Thickness: 32 r.l, ~1.7m.f.p Schematic Side View of CALET SciFi/W Imaging Calorimeter (IMC):  Area: ~ 0.8 m 2  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 m 2  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

11. Sep. 14, 2007TAUP0711 Examples of Simulation Events

12. Shower Profiles by Simulation Gamma-ray 20 MeV Gamma-ray 100MeV Gamma-ray 1GeV Gamma-ray 10GeV Electron 10 GeV Electron 100 GeV Electron 10 TeV Proton 3 TeV pair creation shower

13. Sep. 14, 2007TAUP0713 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 Payload GBM MDP VSC GBM: Gamma-Ray Burst Monitor VSC: Visual Sky Sensor MDP: Mission Data Processor ACD:Anti-coincidence Detector SIA: Silicon Pixel Array IMC: Imaging Calorimeter TASC: Total Absorption Calorimeter

14. Sep. 14, 2007TAUP0714 Details 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

15. Sep. 14, 2007TAUP0715 Detector Development SciFi Belt 64-anode PMT FEC ( VA32, TA, 16bits ADC, FPGA) BGO Si PIN Photodiodes FEC with PD BGO SciFi Belt PMT FEC BGO FEC PD - - -

16. Sep. 14, 2007TAUP0716 Gamma- ｒ ay Burst Monitor Energy Range: 7keV- 20 MeV

17. Sep. 14, 2007TAUP0717 CALET launched by HTV CALET HTV ISS Approach to ISS Pickup of CALET H-IIA Transfer Vehicle （ HTV) Launching of H-II Rocket Separation from H-II Launching Procedure of CALET CALET

18. Sep. 14, 2007TAUP0718 CALET Timeline Proposal AO Selection (3 missions) Selection for Development Phase (Concentrate to one mission) Development Phase Definition CALET Launch Conceptual DesignPreliminary Design Critical Design Maintenance Design & FM Integration Mission Definition SDR Phase A/B Phase C/D Development Phase Definition Phase BBM EM/PM FM (Int’l Partners’ Components) PFM/FM (system level) 1 st round Utilization 2 nd round Utilization SEDA, MAXI(J)SMILES(J) RAID/HICO(US) 2J/AHTV#1HTV#2HTV#3HTV#4HTV#5 TBD (CALET) (Review of progress)

19. Sep. 14, 2007TAUP0719 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 selection expected after two years. * ) This work is supported by a part of “Ground-based Research Announcement for Space Utilization” promoted by Japan Space Forum Summary and Future Prospect

20. Sep. 14, 2007TAUP0720 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 = bE 2 T(Age ） = 1/bE R(Distance)=(2DT) ½ 1 TeV Electron Source: Age < 10 5 years Distance < 1 kpc Vela Cygnus Loop Monogem or Unobserved Sources? Ec=∞ Ec=20TeV Ec=10TeV Electron Density Equation Anisotropy Nearby Source Candidates

21. Sep. 14, 2007TAUP0721 Model Dependence of 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

22. Sep. 14, 2007TAUP0722 Cosmic-Ray Electron Energy Spectrum PPB-BETS The number of electron candidates = 84 events ECC ATIC BETS E 3 ×J Spectrum New Sources ?

23. Sep. 14, 2007TAUP0723 JEM (KIBO) PM & EF JEM PM (Pressurized Module) GPS Antenna JEM 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-Orbit Communication System) JEM ELM-ES (Experiment Logistics Module Exposed Section) JEM will be completed in 2009

24. Sep. 14, 2007TAUP0724 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.