The CALET Mission for Detection of Cosmic Ray

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　　　　 Sep. 14, 2007 TAUP 07 　 Sep. 14 th 2007

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. Baｒbier 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 Sep. 14, 2007 TAUP 07 2

CALET: CALorimetric Electron Telescope Cosmic Rays & Gamma Rays Pulsar SNR Dark Matter AGN International Space Station Japanese Experiment Module (Kibo) CALET Objectives　 p Cosmic Ray Origin and Propagation p p Gamma-ray Sources Dark Matter Gamma-ray Bursts Solar Physics Sep. 14, 2007 TAUP 07 CALET 3

CALET Overview JEM/EF CALET Mission Concept p Observation: Ø Electrons in 1 Ge. V - 10 Te. V ØGamma-rays in 20 Me. V -　* Te. V + Gamma-ray Bursts in 7 ke. V - 20 Me. V Ø P-Fe in several 10 Ge. V - 1000 Te. V CALET p Launch: HTV: H-IIA Transfer Vehicle p Attach Point on the ISS: Exposed Facility of Japanese Experiment Module (JEM-EF) p Life Time: 3(min. ) - 5 years p Mission Status Phase A/B Study Launch around 2013 in Plan Sep. 14, 2007 CALET Payload Ø High Energy Electron and Gamma- Ray Telescope Consisted of - Imaging Calorimeter - Total Absorption Calorimeter Ø Weight: 1500 kg Ø Geometrical Factor: ~0. 7 m 2 sr Ø Power Consumption: 640 W Ø Data Rate: 300 kbps TAUP 07

Purposes of Electron　Observation Search for the signature of nearby flux Search for anisotropy in HE electron HE Precise measurement of electron spectrum Observation of electron spectrum in electron sources (believed to of accele. Expectedof study of a sources. aboveeffectforthe nearbymodelbe SNR) as an 10 Ge. V to define. Spectrum by 1~10 Ge. V Electron solar modulation in theand propagation. ration. CALET Observationabove years the electron spectrum for 3 ~ Te. V (~ 1000 m 2 sr Possible Nearby Sources • T< 105 years • L< 1 kpc Vela 10, 000 years 820 ly Chandra day) 　 W=1048 erg/SN I(E)=I 0 E-α Ｎ=1/30 yr D=D 0(E/Te. V)0. 3 Anisotropy ROSAT Cygnus Loop 20, 000 years 2, 500 ly Monogem 86, 000 years 1, 000 ly Sep. 14, 2007 TAUP 07

Dark Matter Search by Positrons ( & Electrons ) 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 Ge. V KK DM H. C. Cheng et al. , PRL 2002. Direct decay to e+ e- Sep. 14, 2007 TAUP 07 6

Gamma-Ray Observation in 20 Me. V~several Te. V 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 Me. V- 10 Ge. V 　　 l Sky coverage of 70 % for one day ⇒　　 l All sky coverage in 20 days l Typical exposure factor of ~50 days in one year for point source Excellent Energy Resolution ( < a few %) over 100 Ge. V 　　⇒　 l Measurement of change of power-law spectral index l Possible detection of line gamma-rays from Neutralino annihilation Energy Resolution SΩ~5000 cm 2 sr better than GLAST over 10 Ge. V Sep. 14, 2007 TAUP 07

SUSY Dark Matter Search by Gamma-ray Line p WIMP Mass Limit from Direct Observation l l l WIMP mass is likely heavier than ~100 Ge. V Future accelerator experiments will cover the mass range in 100~1000 Ge. V Indirect observation is very promising to see gamma-ray line according to WIMP mass. p CALET Observation of SUSY Dark Matter l l Neutralino annihilating to γγ Maximal annihilation rate of σｖ in L. Bergstorm et al. PRD (2001) Gamma-ray line sensitivity toward the Galactic center (300〇

Origin and Propagation of Proton and Nucleus - Supernova Shock Acceleration Change of power spectrum index depending on Z ? - Propagation in the Galaxy P & He Leaky box model ? Measurements of proton and heavy ion flux in the energy region exceeding 1 Te. V, in which magnet spectrometer is not capable. 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 (Te. V) 1 10 1000 B/C Ratio Number ~106 2. 3 × 104 4. 1 × 102 ~10 Energy Resolution: ~30% , E > 100 Ge. V Sep. 14, 2007 TAUP 07 Heavy Nuclei

Conceptual Structure of CALET Requirements: Ø Large Acceptance and Long Exposure: ~1000 m 2 sr day Ø Shower Imaging Capability: < 1 mm Ø Hadron Rejection Power: > 105 Ø Energy Measurement: 20 Me. V~10 Te. V for e, g several 10 Ge. V ~ 1000 Te. V for hadrons Schematic Side View of CALET ･Anti-Coincidence Detector for Low E. γ ･Silicon Array for High Z and Particle ID Detector Weight: 1450 kg Total Absorber Thickness: 32 r. l, ~1. 7 m. f. p Sci. Fi/W Imaging Calorimeter (IMC): Ø Area: ~ 0. 8 m 2 Ø Sci. Fi Belt: 1 mm square x ~1 m length 17 layers (x &y) ØTungsten Thickness：　4 r. l , 0. 15 m. f. p Total Absorption Calorimeter (TASC): Ø Area: ~0. 36 m 2 Ø BGO Log: 25 x 300 mm 6 layers (x & y) Ø Thickness: 28 r. l , 1. 5 m. f. p Sep. 14, 2007 TAUP 07 10

Examples of Simulation Events Sep. 14, 2007 TAUP 07 11

Shower Profiles by Simulation Gamma-ray 20 Me. V Electron 10 Ge. V Proton 3 Te. V pair creation Gamma-ray 100 Me. V Electron 100 Ge. V pair creation Proton 3 Te. V Gamma-ray 1 Ge. V Electron 10 Te. V shower Gamma-ray 10 Ge. V shower Sep. 14, 2007 TAUP 07 12

Schematic Structure of the CALET Payload ACD: Anti-coincidence Detector SIA: Silicon Pixel Array IMC: Imaging Calorimeter TASC: Total Absorption Calorimeter GBM アンチコインシデ ンスディテクタ (ACD)) ACD VSC MDP イメージング カロリーメータ (IMC) IMC GBM: Gamma-Ray Burst Monitor VSC: Visual Sky Sensor MDP: Mission Data Processor Sep. 14, 2007 SIA シリコンアレイ (SIA) トータルアブソープ ションカロリーメータ (TASC) TASC TAUP 07

Details of Each Component IMC: Imaging Calorimeter TASC: Total Absorption Calorimeter ACD: Anti-Coincidence Detector SIA: Silicon Pixel Array One pixel: 11. 25 mm x 11. 25 mmx 0. 5 mm l 6400 pixels array x 2 layers l Charge resolution: 0. 1 e for p, 0. 35 e for Fe （by Siena U. and Florence U. ) l Sep. 14, 2007 TAUP 07 Segmented Plastic Scintillators (by NASA/Goddard)

Sci. Fi Belt Detector Development 64 -anode PMT Sci. Fi Belt PMT FEC ( VA 32, TA, 16 bits ADC, FPGA) FEC BGO Si PIN Photodiodes PD - - FEC BGO Sep. 14, 2007 TAUP 07 FEC with PD

Gamma-ｒay Burst Monitor Energy Range: 7 ke. V- 20 Me. V Sep. 14, 2007 TAUP 07

Launching Procedure of CALET H-IIA Transfer Vehicle（HTV) CALET launched by HTV ISS Pickup of CALET HTV Approach to ISS HTV Launching of H-II Rocket Separation from H-II CALET Sep. 14, 2007 TAUP 07

CALET Timeline Phase Definition AO Proposal Selection (3 missions) Selection for Development Phase (Concentrate to one mission) Conceptual Design Preliminary Mission Definition Design (Review of progress) SDR Definition Phase CALET Launch Development Phase C/D Phase A/B Development Maintenance Design & FM Integration Critical Design BBM EM/PM PFM/FM (system level) FM (Int’l Partners’ Components) 1 st round Utilization 2 J/A HTV#1 HTV#2 SEDA, MAXI(J) SMILES(J) TBD RAID/HICO(US) Sep. 14, 2007 TAUP 07 2 nd round Utilization HTV#3 HTV#4 HTV#5 TBD (CALET)

Summary and Future Prospect ü We have successfully been developing the CALET instrument for JEM/EF facility from the experience of balloon experiments. ü The CALET has capabilities to observe the electrons up to 10 Te. V , gammarays in 20 Me. V- several Te. V , proton and heavy ions in several 10 Ge. V 1000 Te. V, for investigation of high energy phenomena in the Universe. ü We have already completed a pre-phase A study within last 6 years*. ü JAXA has selected CALET as one of three mission candidates in May, 2007 for concept study and definition of mission instrument (~Phase A/B). ü 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 Sep. 14, 2007 TAUP 07

Characteristics of Cosmic-Ray Electrons Electron Energy Loss by - Inverse Compton Scattering - Synchrotron Radiation Electron Density Equation Anisotropy Electron Propagation in the Galaxy - Diffusion Process Nearby Source Candidates Energy Loss Rate d. E/dt = b. E 2 T(Age）= 1/b. E ½ R(Distance)=(2 DT) 1 Te. V Electron Source: n Age < 105 years n Distance < 1 kpc Vela Cygnus Loop Monogem Ec=∞ Ec=20 Te. V Ec=10 Te. V Sep. 14, 2007 or Unobserved Sources? TAUP 07

Model Dependence of Nearby Source Effect Ec=∞、 ΔT=0 yr, Do=2 x 1029 cm 2/s Do=5 x 1029 cm 2/s Ec= 20 Te. V Sep. 14, 2007 Ec=20 Te. V、 ΔT=1 -104 yr TAUP 07

Cosmic-Ray Electron Energy Spectrum E 3　×J 　Spectrum The number of electron candidates = 84 events BETS ATIC ECC Sep. 14, 2007 New Sources ? PPB-BETS TAUP 07 22

JEM (KIBO) PM & EF GPS Antenna JEM ELM-PS JEM PM (Experiment Logistics Module Pressurized Section) (Pressurized Module) JEMRMS Main Arm JEMRMS SFA (Small Fine Arm) Air Lock ＨＴＶ Antenna JEM EF (Exposed Facility) ICS (Inter-Orbit Communication System) JEM will be completed in 2009 Sep. 14, 2007 TAUP 07 JEM ELM-ES (Experiment Logistics Module Exposed Section)

International Collaboration Team Institution Current Project Contribution in CALET Co PI NASA/Goddard w/ U. of Denver GLAST, BESS Anti-coincidence Detector Simulations R. E. Streitmatter J. F. Ormes Washington U. ACE, TIGER　 Scintillating Fiber Detector S/C – ISS interface unit W. R. Binns 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 *Detector components in support of TASC development. Tentative assignments: Final decisions to be made during Phase A/B. Sep. 14, 2007 TAUP 07