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
Galactic Center
HESS J1813
HESS J1834
13CO cloud
LSI
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

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

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

6. Micro-quasar LS I
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-quasar LS 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: models by F.Mirabel
Microquasar: rel. electrons (& hadrons) from accretion powered jets
Binary Pulsar: Interaction between outflow disk and pulsar winds
Mirabel 2006

10. Extra galactic sources AGNs
M87

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

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

13. The SSC framework Fossati et al. 1998
Higher Z  Higher source luminosity  Lower IC peak  softer spectrum
X-ray intensity at 1keV
PG μJy z~0.3
Mrk μJy z=0.03
Mrk 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 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

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/

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>0.25 unknown) HESS, MAGIC
Very Soft energy spectrum
the attenuation　by 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