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MAGIC

MAGIC. M.Teshima MPI f ü r Physik, M ünchen (Werner-Heisenberg-Institut) for MAGIC collaboration. MAGIC Telescope. 17 m diameter parabolic reflecting surface (240 m 2 ). Light weight Carbon fiber structure for fast repositioning. high reflective diamond milled aluminum mirrors. IPE.

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MAGIC

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  1. MAGIC M.Teshima MPI für Physik, München (Werner-Heisenberg-Institut) for MAGIC collaboration

  2. MAGIC Telescope 17 m diameter parabolic reflecting surface (240 m2 ) Light weight Carbon fiber structure for fast repositioning high reflective diamond milled aluminum mirrors IPE IPE - 3.5o FOV camera - 576 high QE PMTs (QEmax= 30%) IPE NET CE Analog signal transport via optical fibers 3-level trigger system& 300 MHz FADC system Active mirror control(PSF: 90% of light in 0.1o inner pixel)

  3. Highlights of MAGIC observations in Cycle 1 (last one year) Crab Nebular SZA & LZA LSI+61 303 Micro-Quasar Galactic Center HESS J1813 HESS J1834 13CO cloud GRB050713a GRB050904 (in prompt phase) Mrk421 (0.031) Mrk501 (0.034) IAU Circular #8562 1ES2344(z=0.044) 1ES1959 (0.047) 1ES1218(z=0.18) New Source PG 1553 (Z>0.25) New source

  4. Crab Nebula Preliminary

  5. Galactic Center

  6. HESS J1813-178Dark Particle Accelerator -- SNR

  7. Gamma-Ray Emission Processes

  8. HESS J1834extended source VLA 20cm Radio Molecular Cloud 13CO

  9. TeV micro-quasar LS I +61 303 In periastron In 0.2~0.5 from periastron

  10. LS I +61 303 X-Ray Binary System with Radio jet 26.5 days orbital period Distance ~2kpc

  11. Intensities as a function of orbital phase (26.5days orbital period)

  12. Energy Spectrum LS I +61 303

  13. Extra galactic sourcesAGNs M87

  14. Extragalactic sources PKS2005 PG1553 Spectral Indices of new sources range 3~4 New Sources

  15. Absorption of gamma rays in the universe Pair Creation; γ＋γ  e+ + e-

  16. The SSC framework Higher Z  Higher source luminosity  Lower IC peak  softer spectrum X-ray intensity at 1keV PG 1553 6.5 μJy z~0.3 Mrk421 9.9 μJy z=0.03 Mrk501 9.4 μJy z=0.03 PG1553’s source luminosity ~100 x Mrk 2005 1553 2344 Fossati et al. 1998

  17. Mrk421 (z=0.031)AGN (Blazar)

  18. Mrk501 Giant flare 2005 July 01, IAU Circular #8562 2min resolution Light curve

  19. 1ES1218+304(z=0.182) Soft Energy Spectrum Preliminary

  20. PG 1553(z>0.25unknown) Very Soft energy spectrum the attenuationby pair creation or nature of SSC mechanism MAGIC  Z < 0.58

  21. GRB observation by MAGIC Uniformity GLAST Pulse Duration “long” MAGIC “short” ~10sec GRB trigger Satellite to MAGIC ~20sec MAGIC slewing time

  22. MAGIC made an observation in the period of the main prompt emission!! But we knew later z = 6.3

  23. Summary • MAGIC Sources • We have seen ~15 sources including several new sources • Micro-Quasars are playing an important role as a source of galactic cosmic rays • New 100GeV HBLs show steep spectra • The attenuation by e+- creation • The nature of SSC mechanism • GRB observations • 2 among 9 observations were done in prompt phase • Eventually MAGIC may see VHE gammas from GRBs • Second telescope MAGIC-II is under the construction in La Palma • Next year we will start stereo observation  2 times better sensitivity  number of sources may increase ~50 • HESS and MAGIC people are planning CTA after HESS and MAGIC experiment • 10 times better sensitivity than HESS and MAGIC • 1000 VHE sources in norhtern and southern hemisphere

  24. March 2006

  25. By W.Hofmann ∝Ntel 50hrs ∝Area Background Limited Signal Limited

  26. Kifune’s Plot (my optimistic expectation) ~1000 sources by CTA ~3000 sources by GLAST, AGILE GLAST AGILE

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