1. The High Energy Emission of NGC 1365 and 1H 0419-577 Prague: 2010 DOM WALTON IoA, Cambridge In collaboration with Rubens Reis and Andy Fabian

2. OVERVIEW A (really quick) reminder of disc reflection Describe 'Hard Excesses' and their current interpretations Present a disc reflection interpretation for SUZAKU observations of NGC 1365 and 1H0419-577 Dom WaltonPrague: 2010

3. DISC REFLECTION Dom WaltonPrague: 2010

4. SPOT THE SIMILARITY Dom WaltonPrague: 2010

5. Dom Walton SPOT THE SIMILARITY

6. ARABIAN CAMEL Prague: 2010Dom Walton

7. ARABIAN CAMEL Hump Prague: 2010Dom Walton

8. REFLECTION SPECTRUM Prague: 2010Dom Walton

9. REFLECTION SPECTRUM Hump Prague: 2010Dom Walton

10. HARD EXCESSES? Ratio plots to a powerlaw continuum fit to the 2-4 and 7-10 keV energy ranges Both sources display strong emission above 10 keV Previous authors (Risaliti, Braito, et al. 2009, Turner et al. 2009) have claimed disc reflection models alone cannot reproduce the high energy emission. Prague: 2010Dom Walton

11. MODELLING NGC 1365 We make use of REFLIONX (Ross & Fabian, 2005) to construct a model based on disc reflection, including: A powerlaw continuum Reflection from a partially ionised accretion disc Neutral absorption local to the source Neutral reflection from more distant material Four narrow absorption lines Prague: 2010Dom Walton

12. NGC 1365 χ 2 υ = 278/268 Prague: 2010Dom Walton

13. NGC 1365 This model is physically very similar to that used in Risaliti, Miniutti, et al. 2009. We obtain similar results, e.g. Our reflection model reproduces the high energy emission. This is still consistent with the absorption variability interpretation proposed in Risaliti, Miniutti, et al. 2009.  Iron is over-abundant (~3 times solar)  Most of the emission comes from within a few R G Prague: 2010Dom Walton

14. MODELLING 1H 0419-577 Again, we construct a disc reflection model including: Following the work of Fabian et al. (2005), we split the disc into an inner and outer region: The intrinsic powerlaw continuum Reflection from a partially ionised disc Prague: 2010Dom Walton - emissivity- ionisation

15. 1H 0419-577 χ 2 υ = 405/432 Prague: 2010Dom Walton Disc Reflection

16. 1H 0419-577 We find the source to be in a high flux state, following the definitions of Fabian et al. (2005). The low reflection fraction of ~0.3 is consistent with their light bending interpretation. Most of the emission comes from within a few R G ; rotating black hole? The high energy emission is reproduced. Prague: 2010Dom Walton

17. SUMMARY We have constructed disc reflection models for the spectra of NGC 1365 and 1H 0419-577. They work! Partially covering, Compton thick absorbers are not required. Our model for NGC 1365 remains consistent with the variable absorption interpretation of Risaliti, Miniutti, et al. 2009. 1H 0419-577 continues to behave as expected in the light bending interpretation of Fabian, et al. 2005. Prague: 2010Dom Walton