1. CANAGAROO-II PSR B1509-58 Yamagata Univ. N.Sakamoto , S.Gunji
Tokai Univ.
Y.Miyashita , K.Nishijima , J.Kushida
and CANGAROO Team

2. A.K.Harding(2002), astro-ph/0208421
High-Energy Pulsars
A.K.Harding(2002), astro-ph/
EGRET
Gamma-ray pulsars
X-ray & Radio
pulsed emission
detected
X-ray
pulsed emission
detected

3. Gamma-Ray Pulsars •Geminga(J0633+1746) 1.0*10^35 Unable to observe
E / 4πd^2 (arbitrary unit)
•Crab(B ) *10^ Detected
•J *10^ Unable to observe
•Vela(B ) *10^ Detected
•Geminga(J ) *10^ Unable to observe
•B *10^ Marginally Detected
with 3.8m
and ? with 10m
•B *10^ Detected
•B *10^ Unable to observe
•B *10^ ?
•B *10^ ?
•B *10^ Upper limit

4. Timing Analysis of the pulsar
Polar Cap Model
The emission from near the magnetic pole.
Because strong magnetic fields cause pair creation for
high energy gamma rays, gamma rays more than 10 GeV
will not be emitted.
Outer Gap Model
The emission from near the light cylinder.
Because the magnetic fields are not so strong near the light
cylinder, gamma rays up to 100 GeV
would be emitted.
The threshold of ~100 GeV is necessary to distinguish
the two models.

5. PSR B1509-58 and SNR MSH15-52 Source Position(J2000)
(RA , Dec)=(228.48°, °)
Period : ms
Period Derivative :
1540.0×10-15s s-1
Age : 1700 yr
　　SNR MSH15-52
Distance : 4.4 kpc
0.6 ° × 0.5 °
Age : ×103 yr
Magnetic field : 5 ~ 10µG
Over 10 times weaker than Crab
Chandra（2000）
　18´ × 37.5´
Over 10 times wider than Crab

6. PSR B1509-58 spectrum L.Kuiper et al.,A&A(1999) pulsed pulsed? break
COMPTEL
pulsed
WELCOME
pulsed?
RXTE
EGRET
OSSE
break
@10-30Mev
Ginga
unpulsed
CANGAROO
ASCA
GeV,TeV region is Interesting!

7. Observation with CANGAROO-II
2002
On source
Off source
May
20 h 56 m
17 h 41 m
June
8 h 05 m
6 h 15 m
July
5 h 48 m
7 h 12 m
Total
34 h 49 m
31 h 08 m
Off set : 0.55 deg(~ 11 May), 0.40 deg(13 May ~)
Maximum Elevation Angle : deg

8. Imaging Atmospheric Cerenkov Technique (IACT)
Fitting the image
to the ellipse shape
Investigating the alpha distribution
for the air showers, we can
recognize whether the object emits
gamma ray or not.
gamma
proton

9. Alpha Plot PRELIMINARY Low Energy Medium Energy High Energy
sumADC =
- 1.1σ(α<15)
4.1σ(α<15)
- 0.9σ(α<15)
PRELIMINARY

10. 0) Applying more advanced method of data selection,
we will improve the quality of the alpha plot.
1) It is important to identify where the gamma rays are
emitted from. So we will carry out the data analysis
for imaging.
2) Now stereo observation is ready !
So we want to observe PSR B with two telescopes.
For such observation, there are two merits ; better angular
resolution and reduction of the background.
They enable us to investigate the morphology in detail and the
pulsation.
3) In the future, if we can construct a telescope with larger area,
the energy threshold will become lower. It will enable us to
distinguish two theoretical models for pulsars; polar cap model
and outer gap model.