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Fermi LAT observation of SNR

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Presentation on theme: "Fermi LAT observation of SNR"— Presentation transcript:

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

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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 )

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14 Thanks


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