1. Strong Gravity Effects: X-ray spectra, timing and polarimetry AC Fabian IoA Cambridge UK With help from Giovanni Miniutti, Josefin Larsson, Jamie Crummy, Gabriele Ponti, Randy Ross and the MCG6 Suzaku team

2. Rapid variability in AGN MCG-6-30-15

3. Emission dominated by innermost regions Orbital frequency at 10r s Vaughan+

4. Accretion makes massive black holes Soltan 82 Mean redshift Radiative efficiency η The comparison of Є from AGN light and the local BH mass density reqired that the efficiency be at least 0.1

5. REAFs Dominate Radiatively efficient accretion flows Dominant mode of SMBH in terms of GROWTH (Soltan-type arguments) Inner radius of rad efficient disc is few R g Much of the radiation emerges within 6R g

6. Clues from spectra and variability X-ray ‘reflection’ gives important clues in the spectrum Variability timescales and spectral changes show different spectral components

7. Components of an AGN (with Galactic absorption)

8. Reflection from photoionized matter (Ross & Fabian 93, 05) Also see Young+, Nayakshin+, Ballantyne+, Rozanska+, Dumont+

9. Schwarzschild Kerr Fabian+89, Laor 90… Dovciak+04; Beckwith+Done05

10. Vary spectral index Add relativistic blurring Soft excess – broad iron line – Compton hump

11. Very Broad Line  Spinning BH Tanaka+ Iwasawa+ Wilms+ Fabian+

12. Galactic Black Hole GX339-4 Very Broad Line  spinning BH Miller+

13. Crummy+05 22 PG QSO +12 Seyf1 Soft Excesses

14. the soft excess in AGNs seems to have a “universal” temperature despite large differences in BH mass, hard spectral shape, accretion rates … (Czerny+03; Gierlinski & Done 04) it could indicate that the process involved is not thermal as usually assumed but rather linked to atomic processes Can be EXPLAINED by REFLECTION (Ross & Fabian 05; Crummy+05) The soft X-ray excess

15. XMM pn + BeppoSAX PDS MCG-6

16. XTE J1650-500 from BeppoSAX (G. Miniutti)

17. SPIN

18. Assumption: measurements of r ms determine (or constrain) a

19. ISCO conjecture Measure R in from spectra  R ISCO  spin? Maybe not, due to B decreasing R in (Begelman & Reynolds, Gammie, Krolik, Hawley…)?? BUT low ionization  thin, slowly accretion disc, which is not plunging, so R in = R ISCO We conjecture that R in measured from iron line is within 1r g of R isco

20. Ark 120 Vaughan+ 04 NO Broad Line (apparently)

21. Cautionary remarks Narrow 6.4~keV components are expected from distant matter Iron line and reflection continuum need to be self- consistent and blurred together Warm, partial, outflow and other absorption components need to be considered Iron abundance could be a factor (high in MCG-6 and some NLS1, low in other objects) Going within 6GM/c 2 = 3R s can make a large difference in increasing the blurring and so making features less obvious, particularly if abundances only less than solar

22. MCG-5-23-16 Suzaku: Reeves+06

23. Cautionary remarks Narrow 6.4~keV components are expected from distant matter Iron line and reflection continuum need to be self- consistent and blurred together Warm, partial, outflow and other absorption components need to be considered Iron abundance could be a factor (high in MCG-6 and some NLS1, low in other objects) Going within 6GM/c 2 = 3R s can make a large difference in increasing the blurring and so making features less obvious, particularly if abundances only less than solar

24. Complex absorption Spectral models can be made for many sources by using complex absorption (partial covering etc) These can be tested/rejected by: higher spectral resolution broader bandwidth variability

25. Constrains absorption by highly ionized species Implies that simple absorption models for red wing do NOT work Young+05 Chandra HETG

26. Armitage & Reynolds

27. How does it vary? Iwasawa+ Shih+ Fabian+ Vaughan+ McHardy+ Uttley+ Reynolds+

28. Spectral changes seen in 10 flux slices MCG-6-30-15

29. Difference spectrum: (High flux)-(Low flux) is a power-law modified by absorption 1 keV10 keV So we know which large scale features are due to absorption Ratio to power-law

30. Vaughan+Fabian 04 Flux-flux variability

31. Variable power-law Quasi-constant reflection- dominated component Schematic picture of the two-component model

32. Light bending model in Kerr spacetime Miniutti et al 03; Miniutti & Fabian 04; earlier work by Matt et al see also Tsuebsuwong,Malzac+06

34. A source of constant intrinsic luminosity will appear to vary if it changes position within the strong gravity regime close to the black hole

35. PLC Fe line PLC and Fe line variability induced by light bending when an intrinsically constant source changes height The Fe line varies with much smaller amplitude hshs Small h = low PLC flux Large h = high PLC flux

36. Reflection – Power-law relation

37. Suzaku Miniutti+06 MCG-6-30-15

40. Hard X-ray variability measured for the first time Suzaku

41. Suzaku difference spectrum MCG-6-30-15

42. XTE J1650-500 during outburst Rossi +05

43. Is it absorption or a line? Fabian+02,04 1H0707

45. NGC4051 (Ponti+06)

46. Rapid spectral variability of NLS1 explained by GR light bending effects if source within 6m 1H0707

47. Conclusions on broad Fe line A consistent model for the broad iron lines seen in some Seyferts and GBH involves both –strong gravitational redshift –and light bending indicating that much of the reflection and thus primary emission is occurring within a few gravitational radii of the event horizon Good evidence from several objects that BH is spinning (Kerr solution necessary)

48. X-ray Polarization

49. Clear broad iron line may need accretion at high Eddington fraction high iron abundance little complex absorption

51. Brightest lines are about 2 ph m -2 s -1 Need sources with high L/L Edd for broad lines (NLS1/GXRB) Typically means BH mass of 10 6 -10 8 Msun or timescales of 100s to 10 4 s. Therefore to study such BH on their intrinsic variability light crossing timescales inner orbital period  effective collecting area at 6 keV of at least ~1m 2 XEUS / CON-X have the potential to maker MAJOR advances

52. Kevin Rauch JHU

53. data model NGC3516 Iwasawa, Miniutti & Fabian 05

54. Dadina+05 Gallo+05 Red+blue shifted iron lines Several other examples

55. MCG-6-30-15 model prediction See poster by Josefin Larsson

56. SUZAKU

57. Suzaku

61. Variability RMS fractional variability spectrum

63. Summary of MCG-6-30-15 observations: A broad Fe line is present in all flux states Fe line red wing suggests a rotating Kerr black hole 1.The broad Fe line Fabian et al 02 Tanaka et al ’95 – Iwasawa et al ’96 - Guainazzi et al ’99 – Wilms et al 01 – Fabian et al 02 …

64. Summary of MCG-6-30-15 observations: A broad Fe line is present in all flux states Fe line red wing suggests a rotating Kerr black hole 1.The broad Fe line A steep emissivity profile is implied (  > 3 ) possibly in the form of a broken power-law The emissivity suggests the presence of a centrally concentrated primary source of hard X-rays Tanaka et al ’95 – Iwasawa et al ’96 - Guainazzi et al ’99 – Wilms et al 01 – Fabian et al 02 …

65. Cyg X-1 low state (Uttley+05) PSD Log-normal fit f P(f)

66. XMM-Newton observations of MCG-6-30-15 in the 2-10 keV band Wilms et al 2002; Fabian et al 2002; Vaughan et al 2002; Fabian & Vaughan 2002; Ballantyne et al 2003; Reynolds et al 2003; Vaughan & Fabian 2004 Understanding the spectral behaviour

67. Light bending model in Kerr spacetime Miniutti et al 03; Miniutti & Fabian 04; earlier work by Matt et al

69. PLC Fe line PLC and Fe line variability induced by light bending when an intrinsically constant source changes height The Fe line varies with much smaller amplitude hshs Small h = low PLC flux Large h = high PLC flux

70. Reflection – Power-law relation

71. XTE J1650-500 during outburst Rossi +05

72. 1H0707 Boller+02; Gallo+04

73. In lowest state the spectrum is almost completely reflection-dominated The reflection component requires strong relativistic blurring (and implies the disc extends down to 2 grav radii) HF LF 1H0439-577Pounds+04; Fabian+05

74. IRAS13224 G Ponti et al (in preparation)

76. NGC4051 G. Ponti et al (MNRAS submitted)

78. Lockman Hole 800 ks XMM-Newton observation Hasinger Streblyanskaya et al 2004