MAGIC M Teshima MPI fr Physik Mnchen WernerHeisenbergInstitut

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

MAGIC Telescope 17 m diameter parabolic reflecting surface (240 m 2 ) high reflective diamond milled aluminum mirrors Active mirror control (PSF: 90% of light in 0. 1 o inner pixel) Light weight Carbon fiber structure for fast repositioning - 3. 5 o FOV camera - 576 high QE PMTs (QEmax= 30%) Analog signal transport via optical fibers IPE IPE NET CE 3 -level trigger system & 300 MHz FADC system

Highlights of MAGIC observations in Cycle 1 (last one year) Crab Nebular SZA & LZA Mrk 421 (0. 031) Galactic Center HESS J 1813 HESS J 1834 13 CO cloud Mrk 501 (0. 034) 1 ES 2344 (z=0. 044) 1 ES 1959 (0. 047) IAU Circular #8562 LSI+61 303 Micro-Quasar GRB 050713 a GRB 050904 (in prompt phase) 1 ES 1218 (z=0. 18) PG 1553 (Z>0. 25) New Source New source

Crab Nebula Preliminary

Galactic Center

HESS J 1813 -178 Dark Particle Accelerator -- SNR

Gamma-Ray Emission Processes

HESS J 1834 extended source VLA 20 cm Radio Molecular Cloud 13 CO

Te. V micro-quasar LS I +61 303 In periastron In 0. 2~0. 5 from periastron

LS I +61 303 X-Ray Binary System with Radio jet 26. 5 days orbital period Distance ~2 kpc

Intensities as a function of orbital phase (26. 5 days orbital period)

Energy Spectrum LS I +61 303

Extra galactic sources AGNs M 87

Extragalactic sources Spectral Indices of new sources range 3~4 PKS 2005 PG 1553 o S w Ne es c r u

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

The SSC framework Higher Z Higher source luminosity Lower IC peak softer spectrum X-ray intensity at 1 ke. V PG 1553 6. 5 μJy z~0. 3 Mrk 421 9. 9 μJy z=0. 03 Mrk 501 9. 4 μJy z=0. 03 PG 1553’s source luminosity ~100 x Mrk 2005 2344 Fossati et al. 1998 1553

Mrk 421 (z=0. 031) AGN (Blazar)

Mrk 501 Giant flare 2005 July 01, IAU Circular #8562 2 min resolution Light curve

1 ES 1218+304 (z=0. 182) Soft Energy Spectrum Preliminary

PG 1553 (z>0. 25　unknown) Very Soft energy spectrum the attenuation　by pair creation or nature of SSC mechanism MAGIC Z < 0. 58

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

MAGIC made an observation in the period of the main prompt emission!! But we knew later z = 6. 3

Summary MAGIC Sources n n n We have seen ~15 sources including several new sources Micro-Quasars are playing an important role as a source of galactic cosmic rays New 100 Ge. V HBLs show steep spectra The attenuation by e+- creation The nature of SSC mechanism n 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 n 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 n n 10 times better sensitivity than HESS and MAGIC 1000 VHE sources in norhtern and southern hemisphere

March 2006

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

Kifune’s Plot (my optimistic expectation) GLAS T AGILE ~3000 sources by GLAST, AGILE ~1000 sources by CTA