Fermi LAT observation of SNRAbdo, 2010

Li, 2010J.H.K.Wu, 2011M.Dalton, 2011

John W.Hewitt, 2009 (a, b)

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

High-light

Do not only trust Fermi team

Use Catalog and possibility to check

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)

2FGL J1303.7-6316c

HESS J1303-631• binary system PSR B1259-63• Extended: ~0.18 deg

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)

• X-ray PWN identified• HESS J1303-631 can now be identified as a• synchrotron underluminous PWN

OH(1720 MHz) masers

• Green Bank Telescope and Very Large Array• Four SNRs are detected with OH masers: G5.4-

1.2, G5.7-0.0, G8.7-0.1, and G9.7-0.0• Two SNRs, G5.7-0.0 and G8.7-0.1, have TeV γ -

ray counterparts• G8.7-0.1 (W30)• W28 (G5.4-1.2, G5.7-0.0)

W28 (G5.4-1.2, G5.7-0.0)

Thanks