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- しまな こいまる
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1
2 AGN SNR Pulsar e P e + χ e - χ JEM-EF ISS CALET CALorimetric Electron Telescope
3 JAPAN Aoyama Gakuin University Hirosaki University Institute for Cosmic Ray Research, University of Tokyo Ibaraki University JAXA/Space Environment Utilization Center JAXA/ Institute of Aerospace and Astronautical Sciences Kanagawa University Kanagawa University of Human Services High Energy Accelerator Research Organization (KEK) STE, Nagoya University National Inst. of Radiological Sciences Nihon University Ritsumeikan University Saitama University Shibaura Institute of Technology Shinshu University Tokiwa University Tokyo Technology Inst. Waseda University Yokohama National University ITALY University of Siena University of Florence & IFAC (CNR) University of Pisa University of Roma Tor Vergata University of Padova Support Agencies JAXA/SEUC Waseda University with JSPS, MEXT ASI USA NASA/GSFC CRESST/NASA/GSFC and University of Maryland CRESST/NASA/GSFC and Unicersity Space Research Association Louisiana State University NASA Washington University in St Louis University of Denver 43 3
4 CGBM/SGM p CGBM/HXM GPSR (GPS Receiver) MDC(Mission Data Controller) CAL / IMC p 650 kg 650 W FRGF (Flight Releasable Grapple Fixture) ASC (Advanced Stellar Compass) CAL / CHD CAL / TASC m 300 kbps Nominal 20 kbps
5 CALET CALET HTV HTV ISS HTV CALET
6 SNR erg 99% SN1987AKAMIOKANDE 1% erg 10% erg 1% erg dn/de E -2 exp(-e/e c ) Log(dN/dE) Ec Log(E)
7 WIMP χχ e +,e
8 WIMP (1) WIMP line Emission (2) WIMP continuum Emission () Monoenergetic: Direct Production of e+e- pair UniformProduction via Intermediate Particles Double Peak Production by Dipole Distribution via Intermediate Particles
9 IC p+/- or K+/- fi m+/- fi e+/
10 Diffusion Model dn ( ) ( be N ) e 2 - D Ne - e = Q dt E E N e (t, r, E) t, r Q b d D D = D 0 D ( E / 5 GeV) d = 2 ~ 5 0 = ~ E 2 [cm s E < -1 ] 5 GeV 5 GeV
11 E -3 PPB-BETS
12 2 de s = -be = bt + = Thomson c B b + w 2 4 ph dt E( t) E0 3m c Ł 8p e ł E 0 E(t) = E 0 / 2 1 t 1 2 = be
13 10 1 3TeV F
14 TeV SNR - T < R < 1 kpc Vela 10, pc 815 Cygnus Loop 20, pc 2, Monogem 86, pc 1,
15 Ec= ΔT=0 yrdo=2x10 29 cm 2 /s Do=5 x cm 2 /s Ec= 20 TeV Ec=20 TeVΔT= yr
16 Adriani et al. (2008) Chang et al. (2008)
17 ATIC + KKDM620GeV boost factor 200 KKDM hidden U(1) H 1.2TeV s arxiv: / PTP 122(2),553,2009 BESS,PAMELA PAMELA ATIC/PPB-BETS 100GeV
18 CALET KK ( 620 GeV) SUSY ( 820GeV) 2 yearsbf=5) or 5 yearsbf=2) 2years BF=40) or 5 yearsbf=16)
19 (10 5 ) (~2 %) 1 TeV ATIC anomaly 1 GeV?? Vela
20 KK DM vs. SNR type (Δt=10 5 year) SNR Type vs. Pulsar (Δt=310 5 year) CALET Observation CALET Observation KK DM SNR Type Pulsar Type SNR Type Source tot 0 t 0 Ł t 0 SNR Type exp(-t)pulsar Type -2 E ln 4 t ln 4 E Q ( t) exp - Q0 ( t) Lspindown = ł t 0 tot ( 1+ t / t ) 2 0 t 0 t
21 CALET2 CALET N.Tateyama (Ph.D Thesis) > 1 TeV Fermi/LAT CALET5 CALET > 1 TeV
22 Detection of High Energy Gamma-rays Performance for Gamma-ray Detection Simulation of Galactic Diffuse Radiation Energy Range 4 GeV-10 TeV Effective Area 600 cm 2 (10GeV) Field-of-View 2 sr Geometrical Factor 1100 cm 2 sr Energy Resolution 3% (10 GeV) Angular Resolution GeV) Pointing Accuracy 6 Point Source Sensitivity 8 x 10-9 cm -2 s -1 ~25,000 photons are expected per one year Observation Period (planned) (5 years) *) ~7,000 photons from extragalactic γ-background (EGB) per one year Simulation of point sources per one year Energy Spectrum Position Position Vela: ~ 300 photons above 5 GeV Geminga: ~150 photons above 5 GeV Crab: ~ 100 photons above 5 GeV
23 E c = 100 Z
24 CALET p He
25 CALET CALET 5 C O Ne Mg Si Fe
26 /(B/C) D ~ E δ TeV /n K B : Diffusion rate near SNR shocks K B =40 ATIC Ti/Fe 1σ 2σ CREAM Leaky Box Model SNR p-p e -,e + Fermi-LAT,HESS CALET 5 Pamelae + /(e + +e - ) SNR B/C K B =20 arxiv: / Phys. Rev. D 80, (2009)
27 p CHD mm 142 X,YPMT p IMC 1 mm X,Y64chPMT 3 r.l. 0.2 r.l r.l.2 p TASC PWO mm r.l.apd/pd CHD IMC 3 r.l. TASC 27 r.l
28 Gamma-ray 10 GeV Electron 1 TeV Proton 10 TeV IMCTASC CHD e
29 SΩ / CHD
30 1 TeV E -2.7 (1~1000TeV) 1.6x10 6 TeV TeV 95% 4 ~2x10 5 (90% C.L.)
31 Anti ANTI TASC TASC DAQ DAQ SIA SIA Battery HV HV IMC IMC
32
33 CALET ATIC, PAMELA, Fermi-LAT, AMS, HESS, ISS-CREAM, DAMPE, GAMMA-400, CREST
34 ATIC-4 ( ) 19 d 10 h 43 m
35 AMS (green stars), HEAT (open black triangles), BETS (open blue circles), PPB-BETS (bluecrosses), emulsion chambers (black open diamonds)
36 Particle Antiproton flux Positron flux Electron flux Proton flux Electron/positron flux Light nuclei (up to Z=6) Light isotopes (D, 3 He) Antinuclei search Energy Range 80 MeV GeV 50 MeV GeV up to 400 GeV up to 700 GeV up to 2 TeV up to 200 GeV/n up to 1 GeV/n (better than 10-7 in antihe/he)
37 Si + W
38 32.3 GV positron
39 PAMELA
40
41
42 Tracker 9 e 1.03 TeV
43 positron fraction
44 ( Rio de Janeiro )
45 Detector Energy Range (GeV) Energy Resolution e/p Selection Power Key Instrument (Thickness of CAL) SΩT m sr day) PPB-BETS % 4000 IMC ~0.42 GeV (> 10 GeV) (Lead: 9 X 0 ) ATIC ~2% 6,000 Thick Seg. CAL 3.08 (+ ATIC4) a few 1000 ( >100 GeV) (BGO: 18 X 0 ) + C Targets PAMELA GeV 10 5 Magnet + IMC (W:16.3 X 0 ) ~1.6 (2 years) FERMI- LAT 20-1, % ( GeV) ( GeV) Energy dep. GF Tracker + ACD + Thin Seg. CAL (W:1.5X 0 +CsI:8.6X 0 ) 770@100GeV 110@TeV (1 year) AMS 1.5-1,000 (Due to Magnet) ~ GeV 10 4 Magnet+TRD+RICH+IMC (x by TRD ) (Lead: 16.7X 0 ) ~100 (?) (1year) CALET 1-20,000 ~2% (>100 GeV) 10 5 IMC + Thick Seg. CAL (W: 3 X 0 + PWO : 27 X 0 ) 220 (5 years)
46 CALET 20 TeV, 10GeV~ 10TeV, 10 GeV ~ 1000 TeV 6 Pre-phase A CALET JEM-EF TeV
2 X-ray 6 gamma-ray 7 1 17.1 0:38m 0:77m nm 17.2 Hz Hz 1 E p E E = h = ch= (17.2) p = E=c = h=c = h= (17.3) continuum continuous spectrum line spectru
1 17 object 1 observation 17.1 X electromagnetic wave photon 1 = c (17.1) c =3 10 8 ms ;1 m mm = 10 ;3 m m =10 ;6 m nm = 10 ;9 m 1 Hz 17.1 spectrum radio 2 infrared 3 visual light optical light 4 ultraviolet
スライド 1
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