1. Fermi LAT observation of SNR
Abdo, 2010
Li, 2010
J.H.K.Wu, 2011
M.Dalton, 2011
John W.Hewitt, (a, b)

2. Kes 17 Kes 17 (G304.6+0.1) 1720 MHz OH maser (Frail et al. 1996)
9.7 kpc (Caswell et al. 1975)
thermal and a small non-thermal contribution -XMM-Newton (Combi et al. 2010)
a middle-aged SNR of (2.8 − 6.4) × 104 yrs
no TeV emission

5. High-light Do not only trust Fermi team
Use Catalog and possibility to check

6. Problem Old back ground model (long time data and old back model)
No source there (even the 2FGL)
CMAP can’t tell anything
Unbinned & binned?
(time, memory and possibility)

7. 2FGL J c

8. HESS J
binary system PSR B
Extended: ~0.18 deg

9. HESS J1303-631 Extended: ~0.18 deg High spin-down power
pulsar: 1.7e36 erg/sec
Young pulsar: 11,000 years
DM Distance: 6.6 kpc (NE2001, Cordes & Lazio)
At this distance, Gamma-rays represent only 3.7% of
pulsar spin down power (i.e. Gamma-ray efficiency)

10. X-ray PWN identified
HESS J can now be identified as a
synchrotron underluminous PWN

11. OH(1720 MHz) masers Green Bank Telescope and Very Large Array
Four SNRs are detected with OH masers: G , G , G , and G
Two SNRs, G and G , have TeV γ -ray counterparts
G (W30)
W28 (G , G )

12. W28 (G , G )

14. Thanks