M.Teshima M.Teshima

MPI fMPI füür Physik, Mr Physik, Münchenünchen

(Werner-Heisenberg-Institut)(Werner-Heisenberg-Institut)

for MAGIC collaborationfor MAGIC collaboration

MAGICMAGIC

MAGIC-I & MAGIC-IIMAGIC-I & MAGIC-II

MAGIC-II is under construction and will becompleted in the fall of the next year

Improve sensitivity by factor of two

New technologiesto lower the threshold energy

17m diameter largest dishHigh resolution cameraUltra fast read out system 300M 2GHzAnalogue signal fiber transmission

Current MAGIC-I Performance

Fast rotation for GRB < 40secsTrigger threshold 40-50GeVSensitivity ~2.5% of Crab (50hrs)Angular resolution ~0.1 degreesEnergy Resolution 20-30%

MAGIC Highlights of MAGIC Highlights of the First Yearthe First Year

Crab NebularSZA & LZA

Mrk421 (0.031)Galactic Center HESS J1813 HESS J183413CO cloud

1ES2344 (z=0.044) 1ES1218 (z=0.18)New Source

1ES1959 (0.047) PG 1553 (Z>0.25) New source

LSI+61 303Micro-QuasarNew Source

Mrk180 (0.045)New source

Mrk501 (z=0.034)

Crab Nebula (PWN)Crab Nebula (PWN)MAGIC observationMAGIC observation

IC emissionSynchrotronemission

Pulsation:Pulsation:MAGIC 2MAGIC 2 upper limits upper limits(preliminary) (preliminary)

Galactic CenterGalactic CenterB.H., SNR, DM?B.H., SNR, DM?

HESS

MAGIC

HESS

MAGIC

HESSObservation

MAGICObservation

Micro-quasarMicro-quasarLS I +61 303LS I +61 303

X-Ray Binary System with radio jet, 26.5 days orbital periodCompanion star: B0 main sequence star ~18M◎, a Be star with a circumsteller discCompact star: Black hole/neutron star < 4M◎

High eccentric orbit (ε~0.7)

Distance ~2kpc

Microquasar Quasars GRBs

TeV micro-quasarTeV micro-quasarLS I +61 303LS I +61 303

near periastron (Φ=0.23) ~0.3 phase orbit after periastron

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

Parades and his colleagues in 2005

MAGIC observation 54hrs in total

LSI+61 303: modelsLSI+61 303: modelsby F.Mirabelby F.Mirabel

Microquasar: rel. electrons (& hadrons) from accretion powered jets

Binary Pulsar: Interaction between outflow disk and pulsar winds

Mirabel 2006

Extra galactic sourcesExtra galactic sourcesAGNs AGNs

M87

Extragalactic sourcesExtragalactic sources

Spectral Indices of new sources range 3~4

Source Redshift Spectral Index Type First Detection MAGIC publication

M87 0.004 2.9 FR I HEGRA data analysis

Mkn 421 0.031 2.2 BL Lac Whipple ApJ submitted

Mkn 501 0.034 2.4 BL Lac Whipple IAU circular #8562

1ES 2344+514 0.044 2.9 BL Lac Whipple drafting

Mkn 180 0.045 3.3 BL Lac MAGIC ApJ Accepted

1ES 1959+650 0.047 2.4 BL Lac Tel. Array ApJ 639 (2006) 761

PKS 2005-489 0.071 4.0 BL Lac HESS

PKS 2155-304 0.116 3.3 BL Lac Mark VI

H1426+428 0.129 3.3 BL Lac Whipple

H2356-309 0.165 3.1 BL Lac HESS

1ES 1218+304 0.182 3.0 BL Lac MAGIC ApJL 642 (2006) 119

1ES 1101-232 0.186 2.9 BL Lac HESS

PG 1553 >0.25 4.0 BL Lac HESS/MAGIC ApJL submitted

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

0 0.1 0.2 0.3 0.4

Redshift Parameter z

Spe

ctra

l Ind

ex

PKS2005 PG1553

New Sources

Absorption of Absorption of Gamma Rays in the UniverseGamma Rays in the Universe

Pair Creation: γ＋ γ e+ + e-

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

0 0.1 0.2 0.3 0.4

Redshift Parameter z

Spe

ctra

l Ind

ex

PKS2005 PG1553

EBL

The SSC frameworkThe SSC framework

Fossati et al. 1998

Higher Z Higher source luminosity Lower IC peak softer spectrumX-ray intensity at 1keVPG 1553 6.5 μJy z~0.3Mrk421 9.9 μJy z=0.03Mrk501 9.4 μJy z=0.03PG1553’s source luminosity ~100 x Mrk

BL Lac objects

1.5

2.0

2.5

3.0

3.5

4.0

4.5

5.0

0.50 1.00 1.50 2.00 2.50 3.00Log (X- ray source Luminosity)

Spe

ctra

l Ind

ex

2005 1553

2344

Mrk501 Giant flare Mrk501 Giant flare 2005 July 01, IAU Circular #85622005 July 01, IAU Circular #8562

2min resolutionLight curve

Mkn 501 (z=0.034)Mkn 501 (z=0.034) flare on 10 July 2005 flare on 10 July 2005MAGIC ObservationMAGIC Observation

Flare on 10 July 2005 Variability about 5 minutes Spectrum shape changes

within minutes IC peak detected?

2mins bin light curve

New source New source Mkn 180 (z=0.045)Mkn 180 (z=0.045)MAGIC ObservationMAGIC 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+304New source 1ES1218+304(z=0.182) MAGIC Observation(z=0.182) MAGIC Observation

B~0.5G, Doppler factor ~15

Soft Energy Spectrum

New source PG 1553New source PG 1553(z>0.25(z>0.25　　 unknown) HESS, MAGICunknown) HESS, MAGIC

Very Soft energy spectrumthe attenuation　 by pair creationor nature of SSC mechanism

MAGIC Z < 0.78 (published)

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

SummarySummary

MAGIC SourcesMAGIC Sources We have seen more than 12 sources including several new sourWe have seen more than 12 sources including several new sour

cesces Micro-Quasars may be playing an important role as a source of Micro-Quasars may be playing an important role as a source of

galactic cosmic raysgalactic cosmic rays New 100GeV HBLs show steep spectraNew 100GeV HBLs show steep spectra

The attenuation by e+- creationThe attenuation by e+- creationThe nature of SSC mechanismThe nature of SSC mechanism

GRB observations GRB observations 2 among 9 observations were done in prompt phase2 among 9 observations were done in prompt phaseEventually MAGIC will see VHE gamma emission from GRBsEventually MAGIC will see VHE gamma emission from GRBs

Second telescope MAGIC-II is under the constructionSecond telescope MAGIC-II is under the construction Next year we will start stereo observation Next year we will start stereo observation 2 times better sensi 2 times better sensi

tivity tivity number of sources may increase up to 30~50 number of sources may increase up to 30~50