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The CALET Mission for Detection of Cosmic Ray Sources and Dark Matter

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. Member List (24 organizations, 74 members).

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The CALET Mission for Detection of Cosmic Ray Sources and Dark Matter

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  1. 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, JapanTAUP 07 Sep. 14th 2007 TAUP07

  2. 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 TAUP07

  3. CALET:CALorimetric Electron Telescope Cosmic Rays & Gamma Rays Dark Matter AGN Pulsar SNR International Space Station Japanese Experiment Module (Kibo) • CALET Objectives • Cosmic Ray Origin and Propagation • Gamma-ray Sources • Dark Matter • Gamma-ray Bursts • Solar Physics CALET TAUP07

  4. JEM/EF CALET 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 m2sr • Power Consumption: 640 W • Data Rate: 300 kbps TAUP07

  5. Vela 10,000 years 820 ly Chandra Anisotropy ROSAT Cygnus Loop 20,000 years 2,500 ly Monogem 86,000 years 1,000 ly • Possible Nearby Sources • T< 105 years • L< 1 kpc Purposes of ElectronObservation 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 Expected Electron Spectrum by the CALET Observation for 3 years (~ 1000 m2 sr day) W=1048 erg/SN I(E)=I0E-α Ｎ=1/30yr D=D0(E/TeV)0.3 TAUP07

  6. 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 GeV KK DM H.C. Cheng et al., PRL 2002. Direct decay to e+ e- TAUP07

  7. Gamma-Ray Observation in 20 MeV~several TeV • 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 CALET 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 　　⇒　 • Measurement of change of power-law spectral index • Possible detection of line gamma-rays from Neutralino annihilation Energy Resolution SΩ~5000cm2sr better than GLAST over 10 GeV TAUP07

  8. 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. • CALET Observation of SUSY Dark Matter • 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<l<60〇, |b|<10〇) , compared to the gamma-ray line flux from Nutralino annihilation. Expected line signal for 3 year observation TAUP07

  9. Origin and Propagation of Proton and Nucleus - Supernova Shock Acceleration Change of power spectrum index depending on Z ? -Propagation in the Galaxy Leaky box model ? Heavy Nuclei P & He Measurements of proton and heavy ion flux in the energy region exceeding 1 TeV, 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 Resolution:~30% , E > 100 GeV B/C Ratio Energy (TeV) Number 1 ~106 10 2.3 × 104 100 4.1 × 102 1000 ~10 TAUP07

  10. 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, g several 10 GeV ~ 1000 TeV for hadrons Schematic Side View of CALET Conceptual Structure 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, ~1.7m.f.p 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

  11. Examples of Simulation Events TAUP07

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

  13. アンチコインシデ ACD ンスディテクタ (ACD)) GBM SIA シリコンアレイ (SIA) VSC イメージング IMC MDP カロリーメータ (IMC) トータルアブソープ TASC ションカロリーメータ (TASC) Schematic Structure of the CALET Payload ACD:Anti-coincidence Detector SIA: Silicon Pixel Array IMC: Imaging Calorimeter TASC: Total Absorption Calorimeter GBM: Gamma-Ray Burst Monitor VSC: Visual Sky Sensor MDP: Mission Data Processor TAUP07

  14. 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 • 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 (by NASA/Goddard) TAUP07

  15. SciFi Belt 64-anode PMT Detector Development SciFi Belt PMT FEC ( VA32, TA, 16bits ADC, FPGA) FEC Si PIN Photodiodes FEC with PD BGO PD - - - FEC BGO BGO TAUP07

  16. Gamma-ｒay Burst Monitor Energy Range: 7keV- 20 MeV TAUP07

  17. CALET CALET ISS HTV HTV Launching Procedure of CALET H-IIA Transfer Vehicle（HTV) CALET launched by HTV Pickup of CALET Approach to ISS Separation from H-II Launching of H-II Rocket TAUP07

  18. Selection (3 missions) Proposal Selection for Development Phase (Concentrate to one mission) AO Conceptual Design Preliminary Design Critical Design Maintenance Design & FM Integration Mission Definition CALET Launch (Review of progress) Phase Definition SDR Definition Phase Development Phase Phase C/D Phase A/B BBM PFM/FM (system level) EM/PM Development FM (Int’l Partners’ Components) 1st round Utilization 2nd round Utilization 2J/A HTV#1 HTV#2 HTV#3 HTV#4 HTV#5 SEDA, MAXI(J) SMILES(J) RAID/HICO(US) TBD TBD TBD (CALET) CALET Timeline TAUP07

  19. Summary and Future Prospect • 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 TAUP07

  20. Characteristics of Cosmic-Ray Electrons Electron Density Equation Electron Energy Loss by - Inverse Compton Scattering - Synchrotron Radiation Electron Propagation in the Galaxy - Diffusion Process Anisotropy Nearby Source Candidates Energy Loss Rate dE/dt = bE2 T(Age）= 1/bE R(Distance)=(2DT)½ • 1 TeV Electron Source: • Age < 105 years • Distance < 1 kpc Vela Cygnus Loop Monogem or Unobserved Sources? Ec=∞ Ec=20TeV Ec=10TeV 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 TAUP07

  22. E3×J Spectrum The number of electron candidates = 84 events BETS ATIC ECC New Sources ? PPB-BETS Cosmic-Ray Electron Energy Spectrum TAUP07

  23. GPS Antenna JEM ELM-PS (Experiment Logistics Module Pressurized Section) JEM PM (Pressurized Module) JEMRMS Main Arm JEMRMS SFA (Small Fine Arm) Air Lock ＨＴＶ Antenna JEM EF (Exposed Facility) JEM ELM-ES (Experiment Logistics Module Exposed Section) ICS (Inter-Orbit Communication System) JEM (KIBO) PM & EF JEM will be completed in 2009 TAUP07

  24. International Collaboration Team 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, TIGERScintillating 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 *Detector components in support of TASC development. Tentative assignments: Final decisions to be made during Phase A/B. TAUP07

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