S. Aoki Kobe University OPERA Emulsion Workshop 2006/12/09 Gamma-ray Telescope

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Transcript of S. Aoki Kobe University OPERA Emulsion Workshop 2006/12/09 Gamma-ray Telescope

  • Slide 1
  • S. Aoki Kobe University OPERA Emulsion Workshop 2006/12/09 Gamma-ray Telescope
  • Slide 2
  • Photon Observation (pointing) Radio IR Visiblerefrectable optical imaging UV X-ray MeV-Compton scattering multi-Compton scattering GeV-pair creation initial e-track measurement TeV-air shower erenkov light imaging The best tracking detector becomes the best GeV- telescope.
  • Slide 3
  • 2 mrad Current Situation in various wavelength range ex. Crab nebula (M1) Radio (VLA) Infra Red (2MASS) Visible (Palomar) Ultra Violet (UIT) X-ray (Chandra) TeV Gamma (HESS) GeV Gamma (EGRET) 30 mrad 100 mrad a lot of room to improve for GeV-
  • Slide 4
  • Converter Emulsion metal foil spacer Energy Measure ( Em + Pb ) Fiber Tracker ( X and Y ) Emulsion hybrid Gamma-ray Telescope Unit size is about 1 m 2 according to EGRET, Crab = 43 ev / 6hour m 2 (E > 1GeV) Loaded on the Scientific Balloon ($0.1M/flight
  • Energy Measurement E < 700 MeV (beam halo) E > 700 MeV
  • Slide 20
  • Slide 21
  • x 0.1 GeV 1 GeV 10 GeV Angular Resolution (simulation) 68% 95% 68% readout error 0.3 m
  • Slide 22
  • x 0.1 GeV 1 GeV 10 GeV Angular Resolution (simulation) 68% 95% 68% readout error 0.1 m
  • Slide 23
  • Signal to Background estimation According to EGRET (ApJ.494, p734, 1998), Crub Flux = 2.0 10 7 photons cm 2 sec 1 (@E > 1.0GeV) During 24 hours flight, Crab is above the detector 6 hours with 45 aperture # of arriving photon is 43 photons with 1m 2 area. # of Signal event will be 21 ev. with 50% X 0 depth. According to BETS, atmospheric gamma-ray flux is 63 photons m 2 sec 1 sr 1 (@E > 1.0GeV, 25g/cm 2 height) 1.3 10 3 photons cm 2 sec 1 sr 1 (@E > 1.0GeV, 5g/cm 2 height) In the size of Crab nebula (1 1mrad 2 = 4.0 10 6 sr) 1.2 10 9 photons cm 2 sec 1 During 24 hours flight, # of arriving photon is 1.1 photons with 1m 2 area # of Backgound event will be 0.6 ev. with 50% X 0 depth.
  • Slide 24
  • TeV Gamma Observation by HESS (Imaging Air Cerenkov Telescope) PSF 1 Crab nebula (M1) Galactic Sources morphology has become possible TeV Gamma region
  • Slide 25
  • dE/dx measurement dE/dx (a.u.) p ( = 0.79, dE/dx = 1.23 MIP ) ( = 0.99, dE/dx = 1.08 MIP ) OPERA film KEK-PS 1.2 GeV/c beam (29 films)
  • Slide 26
  • momentum (p ) measurement by multiple Coulomb scattering MDM = 5.9 GeV/c with =0.21 m 0 1 2 3 p (GeV/c) p (GeV/c) 1.2 GeV/c 4 GeV/c
  • Slide 27
  • Balloon Flight @ Sanriku 2004/May/30 88.6m MSC (40cm 50cm 8X 0 ) hinge for shifter
  • Slide 28
  • flight path 503km the north latitude the east longitude
  • Slide 29
  • T= 0 T=t T=t 2 shifter to get time information MSC Air-Bag hinge
  • Slide 30
  • altitude [km] shifter displacement [0.1mm] level flight at 36km displacement by atmospheric pressure change air bag #1 air bag #3 air bag #2 (slow change) boomerang flight at 14km Flight Altitude vs. Displacement
  • Slide 31
  • expected track density vs. displacement @0km before launch FLUX=10 -2 cm2/sr/sec T=6.5day=5.6x10 5 sec W=0.5sr(