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Gamma-ray Mapping of the Interstellar Medium and Cosmic Rays in the Galactic Plane with GLAST

Gamma-ray Mapping of the Interstellar Medium and Cosmic Rays in the Galactic Plane with GLAST. Yasushi Fukazawa 1 , T. Kamae 1,2 , T. Ohsugi 1 , T. Mizuno 1 , S. Yoshida 1 , K. Hirano 1 , M. Ozaki 3 , and GLAST team. (1:Hiroshima University, 2:SLAC, 3:ISAS).

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Gamma-ray Mapping of the Interstellar Medium and Cosmic Rays in the Galactic Plane with GLAST

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  1. Gamma-ray Mapping of the Interstellar Medium and Cosmic Rays in the Galactic Plane with GLAST Yasushi Fukazawa1, T. Kamae1,2, T. Ohsugi1, T. Mizuno1, S. Yoshida1, K. Hirano1, M. Ozaki3, and GLAST team (1:Hiroshima University, 2:SLAC, 3:ISAS) GLAST, the next gamma-ray satellite, will be launched in 2005 under USA, Japan, Italy, France, and so on. New ｔechnologies, such as silicon-strip detectors developed in Hiroshima University, enable us to obtain a much imporoved capabilities for gamma-ray observations; 50 times as good as sensitivity as EGRET, good source location down to a few arcmins, and a wider field of view with 20% of the whole sky. Thanks to these characteristics, GLAST will detect more than 10,000 objects. Together with Gamma-ray bursts, Pulsars, BLAZARs, SNRs, Dark matters, the mapping of the Galactic diffuse gamma-ray emission is one of key sciences. This enables us to obtain the distribution of the interstellar medium and cosmic rays in the Galactic plane, especially of protons. We are now developing not only FM silicon-strip detectors but also instrumental simulators which will help us to perform such complex analyses.

  2. 1 1967 OSO-3 SAS-2 1972-73 COS-B 1975-1982 Increase of number of detected objects EGRET (CGRO) 1991- 2000 GLAST will detect >10,000 gamma-ray sources. Various kinds of astronomical objects can be observed, and thus GLAST will open a new era of gamma-ray astronomy. 2005- EGRET GLAST GLAST

  3. 2 Si -Pb Tracker （ＴＫＲ） 4x4 array of identical towers Plastic-Scinti + PMT Anti-Coincidence Detector（ＡＣＤ） PD readout CsI-Array Calorimeter（ＣＡＬ） New Technology Silicon-Strip Detector (FM) Developed by Hiroshima Univ. and HPK (Japan) 9cm

  4. 3 Basic Performance of GLAST EGRET GLAST EGRET GLAST Energy Band 30MeV--10GeV 20MeV--100GeV Field of View 0.5sr 2.4sr (20% of 4π) Effective Area 1,500cm2 11,000cm2 Energy Resolution 10% 10% Dead time per 1 event 100ms 20μs Source Location 5--30arcmin 0.5--5 arcmin Sensitivity ～1×10-7cm-2s-1 ～1×10-7cm-2s-1(1day) ～2×10-9cm-2s-1(2years) Number of Detected objects271 >10000 Weight 1820kg 2560kg Orbit(28.5O incl.) 350km 550km Life time 9years >5yesrs

  5. 4 GLAST is also important as All-sky Monitor Sky covering Wide field of view （20% of the whole sky） can cover 85% of the whole sky in 1orbit (100min) １００sec 1orbit 200 Gamma-ray Bursts per year １day 104 sources in 2 years Day-scale light curve will be available for all 3EG sources + 80 new sources GLAST and MAXI (Japanese X-ray all-sky monitor, 2005-) cooperation will be important.

  6. 5 One of key sciences of GLAST is the Diffuse Gamma-Ray Emission along the Galactic Plane. Gamma-ray is emitted by the interaction between the interstellar medium and cosmic-rays. 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) We can study energy density and distribution of Cosmic-ray Proton, Electron, and Gas (and B), separately, and study the Galactic Structure and Formation in terms of Energetics ! 0 decay(p) π COS-B (Mayer-Hasselwander et al. 1982) Inverse Compton (e) Bremss(e) 100MeV 100GeV

  7. 6 Identify the cosmic-ray acceleration sites. Pulsar nubula Multi-wavelength images of the Galactic plane Evidences of particle acceleraton in the supernova remnant SN1006. From top, 408MHz（Synchrotron）、21cm(H1)、 CO(H2)、FIR（dust,HI）、NIR・optical(stars)、 Ｘ-ray（hot gas） Koyama et al. 1995 Tanimori et al. 1998 EGRET image (left) and GLAST Simulation of the Gamma-Cyg where supernova remnant and molecular cloud are thought to be interacting.

  8. 7 Non-biasing survey of the interstellar gas and cosmic-ray protons and electrons! Combined with other wavelength data, we can obtain the distribition of various Galactic materials. Galaxy radiation simulator But, Extended emission Complex Detector Responses Scanning observation Simulated gamma-ray spectrum of the Galactic plane with GLAST (2x2degre2) ＥＧＲＥＴ image of the giant molecular cloud Forward method anlysis with full-detecor and BGD simulator is valuable and efficient. Orion Digel et al. 1999 Comparison of cosmic-ray density with other galaxies ＳＭＣ M31 LMC (EGRET detected) Clusters of galaxies Starburst Galacy: Ｍ８２ GLAST simulation

  9. 8 We are now developing ….. Cosmic-ray generator for BGD simulation Detector simulator (Geant4) Electrons Protons These are at first applied to the Balloon flight experiments (see postar p210). Further works... Extention to FM model, include He, e+, gamma-ray etc. Tuning through calibrations, study of BGD rejection

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