SUMMARY

1. SUMMARY PROBING STRONG GRAVITY IN AGN Kirpal Nandra Imperial College London

2. PROBING STRONG GRAVITY • The Promise • The Probes • The Progress • The Problems • The Prospects • Probably… Paul Reviews Observations (and Theory)

3. THE PROMISE What are the processes close to the event horizon? Are black holes in AGN spinning? How does BH spin evolve on the Cosmic Scale? How does matter behave in the strong field? Does it obey the predictions of GR?

4. THE PROBES (Iwasawa, Ballantyne, Guainazzi, de la Calle, Svoboda, Miniutti) • Broad emission lines • Narrow emission lines • Narrow absorption lines • Variability/reverb. • Broadband/disk/reflection spectra • Polarimetry • Binary Black Holes • Microlensing (Cappi, Reeves,) (Cappi) (Zoghbi, de Marco, Ponti, Goosmann) (Laor, Walton) (Dovciak) (Komossa, Liu) NOBODY! + Nikolajuk: TBC

5. PROBES: MICROLENSING MICROLENSING! Chartas et al. 2009 Dai et al. 2009 RX J1131-123116 Direct measurement of size of emission region: X-rays from 10 Rg (Optical 70 Rg)

6. THE PROGRESS

7. PROGRESS: INFLOWS/OUTFLOWS NGC1365 Risaliti et al. 2005 (See also Krongold et al. 2007 on NGC4051) Variability allows to place limits on location, mass, etc. Cappi Mrk 509 (long-look, 200ks) Obs1 Obs2 Obs3 MC et al., 2009 Dadina et al. ‘05

8. PROGRESS: HOTSPOTS Cappi, Iwasawa, Reeves, De Marco Iwasawa et al. 2004 Turner et al. 2005

9. PROGRESS: THE INNER FLOW Iwasawa Nikolajuk

10. PROGRESS: BROAD LINES 45% of XMM-Newton Seyfert sample with >30,000 counts Nandra et al. (2007) De La Calle, Guainazzi

11. PROGRESS: BROAD LINES Zoghbi

12. PROGRESS: SPIN MEASUREMENT Ifη implies a* Fanidakis et al. arXiv:0911.1128 Laor: disk continuum fitting

13. PROGREES: SPIN MEASUREMENT Miniutti: broad emission lines Fairall-9 SWIFT J1247 Implications for black hole accretion/merger history through cosmic time (also Ballantyne)

14. PROGRESS: STRONG GRAVITY Iwasawa Walton Svoboda

15. THE PROBLEMS • Broad lines • Predicted to be universal, but not always observed • Degenerate with complex absorption • Lines are much weaker than we might have hoped • Sometimes variable, sometimes now • Narrow lines • NOT predicted unless extreme anisotropic effects. • Limited statistical significance (Vaughan & Uttley) • “Spallation” of Fe • Non-repeatable observations -> cannot test models • Should be transient (Kepler timescale) – is this too convenient? • QPOs • Finally one decent AGN example (RE 1034; Middleton) • Ooops it went away (Middleton) • Which QPO to associate with GBHC? • Interpretation in GBHC not clear despite vastly better data • Overall, two major problems: • Repeatability of observations • Prediction and testing of models

16. PROBLEMS: BROAD LINES Zoghbi Absorption highly unlikely to be sole explanation, but details (e.g. spin) very hard to disentangle

17. PROBLEMS: BROAD LINES 30% of Sample Why are broad lines absent? (Almost) unavoidable prediction of accreting systems… Ionization, Fe abundance, Extreme blurring? Criteria: <99% significance for blurred reflection 12 total: IC4329A (1) NGC 5506(1), NGC 5548(1) NGC 7469(1) Disk line upper limits typically 50-100 eV K. Nandra: broad lines in AGN

18. 6.7 PROBLEMS: S/N RATIO De la Calle

19. PROBLEMS: NARROW FEATURES • Lines statistical significance? (transient features, number of trials in time and energy, etc…) • Identifications of edges/lines energies? (Kallman et al. 2005, Kaspi et al. for PG1211) • Local “contamination”? (PDS456 at risk? McKernan et al. ’04, ‘05) • Publication bias? Only positive detection, low signif., Vaughan & Uttley ‘08) Outflow v (km/s) Solutions: Large Samples, Systematic analysis: Cappi, de Marco, de la Calle, Ponti cz (km/s)

20. PROBLEMS: NARROW LINES Obs 1 vs Obs2 Reeves Strong narrow K line at 6.4 keV. Constant flux over 3 years. However redshifted but relatively narrow line emission is observed at 5.4 keV and 5.9 keV in 2005 low state.

21. PROBLEMS: NARROW LINES Mostly S. Vaughan Suzaku All XMM co-add 5.4 keV Reeves If 5.4 keV is real, it is variable (thus not spallation)

22. PROBLEMS: LINE VARIABILITY Bhayani & Nandra (2010) Variability key to break degeneracies: Iwasawa, Zoghbi, Reeves, de Marco, Ponti, Goosmann BUT… source behaviour not predictable with current models

23. PROSPECTS: REVERBERATION Zoghbi Reeves

24. PROSPECTS: POLARIZATION X-ray polarimetry: a new window to be opened by GEMS, NHXM, IXO Dovciak

25. PROSPECTS: BH SPIN ASTRO-H: First high resolution, high throughput spectroscopy at 6 keV IXO: ULTRA-HIGH THROUGHPUT ASTRO-H IXO MCG-6-30-15 100ks IXO XMS NGC 3783 300ks IXO

26. PROSPECTS: TRACING HOTSPOTS IXO: high throughput C. Reynolds Flux constraint ~20% 400s exposure: 1/10 tKeplerian at 6 rg

27. PROSPECTS: TESTING GR? Testing the no-hair theorem e=0 GR correct e=0.0 (GR) 0.2 =0.5 C. Reynolds Johanssen & Psaltis (2009)

28. PROGNOSIS • Strong gravity effects in AGN can be probed • For example, mlensing shows X-rays arise within ~10 Rg • Major issues: • Model degeneracies • Unrepeatable observations • Lack of testable model framework • Major progress • Large samples, systematic analysis • Variability studies, reverberation • Huge future potential • High resolution spectroscopy • High throughput spectroscopy • Polarimetry Promising Prospects for Proactive Promotion of Proposed Projects IXO See you in Progue 2020!