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MAGIC

MAGIC. M.Teshima MPI f ü r Physik, M ünchen (Werner-Heisenberg-Institut) for MAGIC collaboration. MAGIC-I & MAGIC-II. MAGIC-II is under construction and will be completed in the fall of the next year Improve sensitivity by factor of two. New technologies to lower the threshold energy

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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-I & MAGIC-II MAGIC-II is under construction and will be completed in the fall of the next year Improve sensitivity by factor of two New technologies to lower the threshold energy 17m diameter largest dish High resolution camera Ultra fast read out system 300M  2GHz Analogue signal fiber transmission Current MAGIC-I Performance Fast rotation for GRB < 40secs Trigger threshold 40-50GeV Sensitivity ~2.5% of Crab (50hrs) Angular resolution ~0.1 degrees Energy Resolution 20-30%

  3. MAGIC Highlights of the First Year Crab Nebular SZA & LZA LSI+61 303 Micro-Quasar New Source Galactic Center HESS J1813 HESS J1834 13CO cloud Mrk421 (0.031) 1ES2344(z=0.044) Mrk180 (0.045) New source 1ES1959 (0.047) 1ES1218(z=0.18) New Source PG 1553 (Z>0.25) New source Mrk501 (z=0.034)

  4. Crab Nebula (PWN)MAGIC observation Pulsation: MAGIC 2 upper limits (preliminary) Synchrotron emission IC emission

  5. Galactic CenterB.H., SNR, DM? HESS HESS HESS Observation MAGIC Observation MAGIC MAGIC

  6. Micro-quasarLS I +61 303 X-Ray Binary System with radio jet, 26.5 days orbital period Companion star: B0 main sequence star ~18M◎, a Be star with a circumsteller disc Compact star: Black hole/neutron star < 4M◎ High eccentric orbit (ε~0.7) Distance ~2kpc Microquasar Quasars GRBs

  7. TeV micro-quasarLS I +61 303 ~0.3 phase orbit after periastron near periastron (Φ=0.23)

  8. Intensities as a function of orbital phase (26.5days orbital period) MAGIC observation 54hrs in total Parades and his colleagues in 2005

  9. LSI+61 303: modelsby F.Mirabel Mirabel 2006 • Microquasar: rel. electrons (& hadrons) from accretion powered jets • Binary Pulsar: Interaction between outflow disk and pulsar winds

  10. Extra galactic sourcesAGNs M87

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

  12. Absorption of Gamma Rays in the Universe EBL PKS2005 PG1553 Pair Creation: γ＋γ  e+ + e-

  13. 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

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

  15. Mkn 501 (z=0.034) flare on 10 July 2005MAGIC Observation • Flare on 10 July 2005 • Variability about 5 minutes • Spectrum shape changes within minutes • IC peak detected? 2mins bin light curve

  16. New source Mkn 180 (z=0.045)MAGIC Observation • New source discovered by MAGIC • April 2006, 11.1 h • 5.5 , F(>200GeV) = 11%C.U., • Soft spectrum index: -3.3 ± 0.7 Subm. to ApJL, astro-ph/0606630

  17. New source 1ES1218+304(z=0.182) MAGIC Observation B~0.5G, Doppler factor ~15 Soft Energy Spectrum

  18. New source PG 1553(z>0.25unknown) HESS, MAGIC Very Soft energy spectrum the attenuationby pair creation or nature of SSC mechanism MAGIC  Z < 0.78 (published)

  19. Distance of PG1553 Test with combined spectrum (Z<0.42 preliminary)

  20. Summary • MAGIC Sources • We have seen more than 12 sources including several new sources • Micro-Quasars may be 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 will see VHE gamma emission from GRBs • Second telescope MAGIC-II is under the construction • Next year we will start stereo observation  2 times better sensitivity  number of sources may increase up to 30~50

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