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The High Energy Emission of NGC 1365 and 1H 0419-577

The High Energy Emission of NGC 1365 and 1H 0419-577. DOM WALTON IoA, Cambridge In collaboration with Rubens Reis and Andy Fabian. Prague: 2010. OVERVIEW. A (really quick) reminder of disc reflection Describe 'Hard Excesses' and their current interpretations

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The High Energy Emission of NGC 1365 and 1H 0419-577

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

  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 Walton Prague: 2010

  3. DISC REFLECTION Dom Walton Prague: 2010

  4. SPOT THE SIMILARITY Dom Walton Prague: 2010

  5. SPOT THE SIMILARITY Dom Walton Prague: 2010

  6. ARABIAN CAMEL Dom Walton Prague: 2010

  7. ARABIAN CAMEL Hump Dom Walton Prague: 2010

  8. REFLECTION SPECTRUM Dom Walton Prague: 2010

  9. REFLECTION SPECTRUM Hump Dom Walton Prague: 2010

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

  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 Dom Walton Prague: 2010

  12. NGC 1365 χ2υ= 278/268 Dom Walton Prague: 2010

  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 RG Dom Walton Prague: 2010

  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 - emissivity - ionisation Dom Walton Prague: 2010

  15. 1H 0419-577 Disc Reflection χ2υ= 405/432 Dom Walton Prague: 2010

  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 RG; rotating black hole? • The high energy emission is reproduced. Dom Walton Prague: 2010

  17. SUMMARY • We have constructed disc reflection models for the spectra of NGC1365 and 1H0419-577. • They work! Partially covering, Compton thick absorbers are not required. • Our model for NGC1365 remains consistent with the variable absorption interpretation of Risaliti, Miniutti, et al. 2009. • 1H0419-577 continues to behave as expected in the light bending interpretation of Fabian, et al. 2005. Dom Walton Prague: 2010

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