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Fermi LAT observation of SNR
Abdo, 2010 Li, 2010 J.H.K.Wu, 2011 M.Dalton, 2011 John W.Hewitt, (a, b)
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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
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High-light Do not only trust Fermi team
Use Catalog and possibility to check
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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)
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2FGL J c
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HESS J binary system PSR B Extended: ~0.18 deg
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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)
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X-ray PWN identified HESS J can now be identified as a synchrotron underluminous PWN
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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 )
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W28 (G , G )
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Thanks
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