Transcript 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.

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
Mrk501 (z=0.034) 1ES2344 (z=0.044) Mrk180 (0.045)
New source
HESS J1834
13CO cloud
LSI+61 303 Mrk421 (0.031)
Micro-Quasar
New Source
1ES1959 (0.047) 1ES1218 (z=0.18) PG 1553 (Z>0.25)
New Source
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
near periastron (Φ=0.23)
~0.3 phase orbit
after periastron
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
Source
Redshift
Spectral Index
Type
First Detection
MAGIC publication
HEGRA
data analysis
M87
0.004
2.9
FR I
Mkn 421
0.031
2.2
BL Lac
BL Lac objects
Whipple
ApJ submitted
4.5
Mkn 501
0.034
2.4
BL Lac
Whipple
#8562
PKS2005IAU circular
PG1553
1ES 2344+514
0.044
2.9
BL Lac
Mkn 180
0.045
3.3
BL Lac
1ES 1959+650
0.047
2.4
BL Lac
PKS 2005-489
0.071
4.0
BL Lac
PKS 2155-304
0.116
3.3
BL Lac
H1426+428
0.129
3.3
BL Lac
H2356-309
0.165
3.1
BL Lac
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
4.0
Spectral Index
Whipple
drafting
3.5
MAGIC
ApJ Accepted
Tel.
Array
3.0
ApJ 639 (2006) 761
HESS
2.5
Mark VI
2.0
Whipple
1.5
HESS
0
0.1
0.2
0.4
0.3
z
Redshift
ApJLParameter
642 (2006)
119
ApJL submitted
Absorption of
Gamma Rays in the Universe
EBL
Pair Creation:
γ＋γ  e+ + eBL Lac objects
4.5
PKS2005
PG1553
Spectral Index
4.0
3.5
3.0
2.5
2.0
1.5
0
0.1
0.2
0.3
Redshift Parameter z
0.4
The SSC framework
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
BL Lac objects
5.0
2005
4.5
1553
Spectral Index
4.0
3.5
2344
3.0
2.5
2.0
1.5
0.50
Fossati et al. 1998
1.00
1.50
2.00
2.50
Log (X-ray source Luminosity)
3.00
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

Flare on 10 July 2005
 Variability about 5 minutes
 Spectrum shape changes
within minutes
 IC peak detected?
2mins bin light curve
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