1 / 14

Fermi LAT observation of SNR

Fermi LAT observation of SNR. Abdo , 2010 Li, 2010 J.H.K.Wu , 2011 M.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)

moya
Download Presentation

Fermi LAT observation of SNR

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Fermi LAT observation of SNR Abdo, 2010 Li, 2010 J.H.K.Wu, 2011 M.Dalton, 2011 John W.Hewitt, 2009 (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

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

  4. 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)

  5. 2FGL J1303.7-6316c

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

  7. 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)

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

  9. 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)

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

  11. Thanks

More Related