MAGIC M.Teshima MPI für Physik, München (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 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%

MAGIC Highlights of the First Year Crab Nebular SZA & LZA Galactic Center HESS J1813 HESS J1834 13CO cloud LSI+61 303 Micro-Quasar New Source Mrk421 (0.031) Mrk501 (z=0.034) 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

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

Galactic Center B.H., SNR, DM? HESS HESS HESS Observation MAGIC Observation MAGIC MAGIC

Micro-quasar LS 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

TeV micro-quasar LS I +61 303 ~0.3 phase orbit after periastron near periastron (Φ=0.23)

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

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

Extra galactic sources AGNs M87

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

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

The SSC framework Fossati et al. 1998 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

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

Mkn 501 (z=0.034) flare on 10 July 2005 MAGIC Observation Variability about 5 minutes Spectrum shape changes within minutes IC peak detected? 2mins bin light curve Fuer QG limits: Tau limitiert auf 50sec+/- 50%, alle 3 symmetrisch

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

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

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

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

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