040308fukazawa.ppt
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1 GLAST X
2 MeV--GeV OSO-3 SAS-2 COS-B EGRET (CGRO) GLAST OSO-III (1967): SAS-2 (1972): 10 COS-B (1975): 3C273 EGRET(1991): E~10GeV BLAZER 5
3 Isolated Neutron Star? CTA 1 SNR? EGRET All Sky Map (>1 GeV) 3C279 (blazar) Vela (radio pulsar) Geminga pulsar LSI +61 o 303 Binary System? g Cygni SNR? unidentified transient Galactic Center? PKS (blazar) LMC Crab pulsar Orion Cloud
4 cm -2 s -1 (2 EGRET GLAST 30MeV--10GeV 20MeV--100GeV ield of View 0.5sr 2.4sr (20% of 4 1,500cm2 11,000cm2 10% 10% 100ms 20 s cm -2 s cm -2 s -1 (1 271 > kg 2560kg 160W 600W rbit(28.5 incl.) 350km 550km 9 >5
5 Delta II Si -Pb Tracker 7920 H Large Area Telescope 2560 kg, 600 W, 1.73² 1.06 m CsI Calorimeter Anti-Coincidence Detector Gamma-ray Burst Monitor
6 4x4 array of identical towers Si-strip Tracker (TKR) 18 XY tracking planes,. CsI Calorimeter(CAL) segmented array of CsI(Tl) with PD Anticoincidence Detector (ACD) (ACD) segmentaed plastic scintillator with PMT background Segmentation Data Acquisition (DAQ) System. 0 MeV GeV.
7 tanford University: SLAC & HEPL ASA Goddard Space Flight Center SFC) S Naval Research Laboratory BL) niversity of California, Santa Cruz CSC) onoma State University (SSU) niversity of Washington (UW) :, ISAS,, : INFN, ASI : CEA/DAPNIA, IN2P3 : KTH Country USA 45 Japan Italy France Sweden Germany 3 ~ 100 collaborators from 28 institutions # Collaborators 15 (T.Ohsugi, TKR) 16 (G.Barbiellini, TKR) 14 (I.Grenier, CAL) 4 (P.Carlson, CAL)
8 : Kemmer et al (late 1970s,,, GLAST
9 VS
10 Tracker Module Mechanical Design by cm 4 4 array of Si-strip sensors (X) C-fiber face shee Hex cell core Al closeout C-fiber face sheet Carbon thermal panel 4 4 array of Si-strip
11 FOV w/ energy measurement due to favorable aspe ratio Expected Performance (after all background rejection cuts) Effects of longitudinal shower profilin
12 GRET 95% 0.5 EGRET 5s LAT source r = 7 LAT 95% 3EG r = 0.3 GLAST
13 EGRET to GLAST EGRET( ) GLAST( ) 271
14 GLAST 1orbit large field-of-view 20% orbit(100 ) 85% 200 g bursts per year 1 3EG limit all 3EG sources + 80 new in sources in 1 survey LAT 1 yr cm -2 s -1
15 TeV GLAST CANGAROO-III
16 Activity(1) Silicon Strip Detectors By and HPK 90% SSDs (9500 ) Flight SSDs Quality dead strip! 0.008% in 9500 SSD 384 strips 3.7M strips 2.5 na/cm 65 V ρ= 9 kωcm
17
18 CAL) Anti ACD CAL ACD
19 Activity(2) GLAST BGD 1000c/s (BFEM): single tower Trigger rate vs. atmospheric depth
20 ( ) AMS our model (used in Geant4 Simulation) BESS (magnetic north pole) FM GLAST ( ( ) ) GeV data eant4 alpha proton charged events
21 GAP onthermal
22 NeXT NeXT Astro-E2 HXD
23 NeXT SGD γ γ E1 BGD E2 BGD
24 Contemporary X-ray Missions NeXT keV INTEGRAL 5keV--5MeV Astro-E kev High sensitivity for diffuse hard X-ray emission High sensitivity above 10 kev Doppler measurement MAXI 2--30keV X-ray mapping of diffuse Galactic X-ray 2010?? keV, Al26 line mapping GLAST 10MeV 300GeV 2007-
25 AGN
26 Non-thermal X SNR BLAZAR.. SNR SNR BLAZAR 511keV
27 kev MeV GeV TeV GLAST( ) X GLAST( ) X-ray X-ray X-ray
28 1km 10 6 km 1pc 1kpc 1Mpc L B G Hillas Emax evbl 10 6 G AGN? ev 1G ev SNR 1 G disk/halo
29 Sources EGRET 3 rd Catalog: 271 sources
30 Pulsars (Rotating Neutron Stars) GLAST will detect >50 pulsars. Gamma-ray emission mechanisms? PolarCap pulsed OuterGap(Unpulsed) EGRETが検出した7つ のパルサーの パルスプロファイル Thompson
31 De Jager Crab ut-off energy (MeV) OuterGap PolarCap GeV
32
33 SNR RXJ Unidentified EGRET Sources (Reimer and Pohl). (Halpern et al., Reimer et al. )
34 New Pulsars (like Geminga) Raio-Quiet Pulsars New discovery of Gamma-ray pulsars (Halperns et al. 2001) PSR J profile? (Torres et al. 2001) PSR J , PSRs J , PSR J , PSR J
35 Koyama et al Tanimori et al Gamma Cyg EGRET GLAST
36 et al. ( ) (Loss flat) -Cygni,W28..
37 Bremss?, Aharonian Bremms by PeV-proton De Jager and Mastichiadis (1997). SNR J (Uchiyama et al.)!
38 Pi-0 decay (cosmic ray p) * (interstellar gas) Bremss (cosmic ray e) * (interstellar gas) IC (cosmic ray e) * (interstellar photon) Radio-synchrotron (cosmic ray e) * (interstellar B) osmic-ray Proton, Electron, and Gas (and B) nergetics 0 decay(p) Inverse Compton Bremss(e) (e)
39 EGRET 0 excess? But high energy cut-off? TeV (Whipple) Proton escape in the outer region? Hunter et al. 199
40 Diffuse thermal RXTE Hard tail Ginga/Balloon powerlaw (kev) (kev) Valinia et al Diffuse 511keV
41 Diffuse Ginga Fe-K Line map Si-K Fe-K ASCA kt=3-5kev Lx=10 38 erg/s (10 4 ev/cm 3 ) SN rate Unknown heating and acceleration mechanisms???
42 X kt=3kev Bremss? GeV 0 Bremss Electron spectrum in-situ acceleration et al.
43 50 Giant Molecular Clouds (D 1kpc, M=10 5 M.) Ophuichus Hunter et al Orion Overall proton distribution 3 3 degree 2 grid mapping e and p distribution Simulated spectra of GLAST
44 Cosmic-ray Conten p and e young SNRs or spiral arm? Proton uniform? Energy equipartition? Energy density distribution of p and e Ionization Accelaration rate LMC simulation (LMC,SMC,M31,M82 ) SMC? clusters of galaxies? (Coma Cluster )
45 For Abell clusters with 1 degree from EGRET sources Proton Electron? (Totani et al.) Dark Matter? Prediction of Gamma-ray emission Pion-decay Annihilation of dark matter Neutralinos Possible correlation? Inverse Compton ohr et al. (2001) gives only upper limits of EGRET
46 X Coma Cluster HCG62 group (kev) Fusco-Femiano 1999 et al Cooling Flow keV NeXT
47 NGC253 Itoh Enomoto Tsuru TeV
48 GLAST.. BLAZER Galactic.. Internal or External?? e+ or p??......
49 RXTE ASM LMC X-1 5 LMC X-3
50 Mrk421 TA TA RXTE 23day RXTE (MJD) (day)
51 time lag Rise time 3C279 X-rays UV Optical IR Radio
52 BLAZER SED Radio Optical X-ray Gamma ray FSRQ LBL HBL
53 SSC Externa Compto e- e- e- GLAST OVV QSO
54
55 TeV Blazar(HBL) OVV QSO
56 FR-II FSRQ GeV FSRQ FR-I LBL ṁṁmṁ. ev LBL FR-I HBL PeV BLAZER SED Radio Optical X-ray Gamma ray HBL
57 GLAST z>6 distant QSO-hostedBLAZAR GLAST supermassive BHs (z=2.0) EGRET detected
58 BLAZAR,
59 Galactic BH X GROJ1655
60 Galactic BLAZER GLAST High State FSRQ GX339-1 SED X X Gallo et al GeV
ガンマ線観測の新時代到来を告げる衛星計画 10MeV-100GeV のガンマ線領域の観測は 1967 年の OSO-3 によって始まり 1970 年代の SAS-2 COS-B によって本格的な観測結果が得られ 1990 年代の EGRET(CGRO 衛星搭載 ) によって大きく前進した 特に CG
次期ガンマ線観測衛星 GLAST (Gamma-ray Large Area Space Telescope) 深沢泰司 釜江常好 大杉節 吉田勝一 水野恒史 ( 広島大学 ) 尾崎正伸 高橋忠幸 (ISAS) 河合誠之 ( 理研 ) 米日伊仏共同 ( 日本 : 広島大学 宇宙研 東京工業大学 理研 ) 極限状態の宇宙を探る ガンマ線観測の新時代到来を告げる衛星計画 10MeV-100GeV のガンマ線領域の観測は
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