M.Teshima M.Teshima

MPI fMPI füür Physik, Mr Physik, Münchenünchen

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

for MAGIC collaborationfor MAGIC collaboration

MAGICMAGIC

MAGIC TelescopeMAGIC Telescope17 m diameter parabolic reflecting surface (240 m17 m diameter parabolic reflecting surface (240 m2 2 ))

Analog signal transport Analog signal transport via optical fibers via optical fibers

IPEIPEIPE

CENET

3-level trigger system3-level trigger system& 300 MHz FADC system& 300 MHz FADC system

Active mirror controlActive mirror control (PSF: 90% of light in (PSF: 90% of light in 0.1 0.1oo inner pixel) inner pixel)

high reflective diamond milled high reflective diamond milled aluminum mirrorsaluminum mirrors

Light weight Carbon fiber structure for

fast repositioning

- 3.5- 3.5oo FOV camera FOV camera - 576 - 576 high QE PMTshigh QE PMTs (QE (QEmaxmax= 30%)= 30%)

Highlights of MAGIC observations in Highlights of MAGIC observations in Cycle 1 (last one year)Cycle 1 (last one year)

Crab NebularSZA & LZA

Mrk421 (0.031) Mrk501 (0.034)IAU Circular #8562

Galactic Center HESS J1813 GRB050713aGRB050904 (in prompt phase)

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-Quasar

Crab NebulaCrab Nebula

Preliminary

Galactic CenterGalactic Center

HESS J1813-178HESS J1813-178Dark Particle Accelerator -- SNRDark Particle Accelerator -- SNR

Gamma-Ray Emission ProcessesGamma-Ray Emission Processes

Uphoton

2

maxTI.C. 3

4 γcdt

dE

23

4 22

maxTSync

B

dt

dE cγ

6.1 E

2.2 E

2.2 E

2.2 E

2.2 E6.1 E

HESS J1834HESS J1834extended sourceextended source

VLA 20cm Radio Molecular Cloud 13CO

TeV micro-quasarTeV micro-quasarLS I +61 303

In periastron In 0.2~0.5 from periastron

LS I +61 303LS I +61 303

X-Ray Binary Systemwith Radio jet

26.5 days orbital period

Distance ~2kpc

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

Energy Spectrum Energy Spectrum LS I +61 303LS I +61 303

Extra galactic sourcesExtra galactic sourcesAGNs AGNs

M87

Extragalactic sourcesExtragalactic sources

Source Redshift Spectral Index Type FirstDetection

Confimation

M87 0.004 2.9 FR I HEGRA HESS

Mkn 421 0.031 2.2 BL Lac Whipple Many

Mkn 501 0.034 2.4 BL Lac Whipple Many

1ES 2344+514 0.044 2.9 BL Lac Whipple HEGRA,MAGIC1ES 1959+650 0.047 2.4 BL Lac Tel. Array Many

PKS 2005-489 0.071 4.0 BL Lac HESS

PKS 2155-304 0.116 3.3 BL Lac Mark VI HESS

H1426+428 0.129 3.3 BL Lac Whipple Many

H2356-309 0.165 3.1 BL Lac HESS

1ES 1218+304 0.182 3.0 BL Lac MAGIC

1ES 1101-232 0.186 2.9 BL Lac HESS

PG 1553 >0.25 4.0 BL Lac HESS MAGIC

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

Spectral Indices of new sources range 3~4

Absorption of Absorption of gamma rays in the universegamma rays in the universe

Pair Creation; γ＋ γ e+ + e-

The SSC frameworkThe SSC framework

Fossati et al. 1998

Higher Z Higher source luminosity Lower IC peak softer spectrum

X-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

Mrk421 (z=0.031)Mrk421 (z=0.031)AGN (Blazar)AGN (Blazar)

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

2min resolutionLight curve

1ES1218+3041ES1218+304(z=0.182)(z=0.182)

Preliminary

Soft Energy Spectrum

PG 1553PG 1553(z>0.25(z>0.25 　　 unknown)unknown)

Very Soft energy spectrum

the attenuation　 by pair creationor nature of SSC mechanism

MAGIC Z < 0.58

GRB observation by MAGICGRB observation by MAGIC

MAGIC

GLAST

Pulse Duration

“short”

“long”

Uniformity

~10sec GRB trigger Satellite to MAGIC~20sec MAGIC slewing time

But we knew later z = 6.3

MAGIC made an observation in the period of the main prompt emission!!

SummarySummary

MAGIC SourcesMAGIC Sources We have seen ~15 sources including several new sourcesWe have seen ~15 sources including several new sources Micro-Quasars are playing an important role as a source of galactic cosMicro-Quasars are playing an important role as a source of galactic cos

mic raysmic 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 may see VHE gammas from GRBsEventually MAGIC may see VHE gammas from GRBs

Second telescope MAGIC-II is under the construction in La PalmaSecond telescope MAGIC-II is under the construction in La Palma Next year we will start stereo observation Next year we will start stereo observation 2 times better sensitivity 2 times better sensitivity

number of sources may increase ~50 number of sources may increase ~50

HESS and MAGIC people are planning CTA after HESS and MAGIHESS and MAGIC people are planning CTA after HESS and MAGIC experimentC experiment

10 times better sensitivity than HESS and MAGIC10 times better sensitivity than HESS and MAGIC 1000 VHE sources in norhtern and southern hemisphere1000 VHE sources in norhtern and southern hemisphere

March 2006

By W.Hofmann

∝Ntel

∝Area50hrs

Background Limited Signal Limited

Kifune’s Plot Kifune’s Plot (my optimistic expectation)(my optimistic expectation)

~3000 sourcesby GLAST, AGILE

~1000 sourcesby CTA

GLASTAGILE