Gabriele Ponti University of Southampton

1. A XMM-Newton study of the Fe K band variability in the 22 brightest-unabsorbed AGN Gabriele Ponti University of Southampton thanks to: G. Miniutti, P. Uttley, L. Gallo, B. De Marco, M. Cappi, A. Fabian, R. Goosmann, A. Goldwurm, R. Terrier, G. Trap, G. Belanger and the FERO collaboration

2. Typical 3-10 keV spectrum of Seyfert 1

3. Typical 3-10 keV spectrum of Seyfert 1 Tanaka et al. 1995; Fabian et al. 2002; Guainazzi et al. 2006; Nandra et al. 2007

4. Typical 3-10 keV spectrum of Seyfert 1 Reeves et al. 2004; Done et al. 2007; Miller et al. 2008 An ionised partially covering absorber may produce a spectral curvature in the 3-10 keV band resembling a broad Fe K line Mean spectra degenerate!  spectral variability

5. The sample of type AGNs: The brightest unabsorbed (NH<1.51022 cm-2) AGNs from the RXTE Slew Survey(Revnivtev et al. 2004) Subsample of Guainazzi et al. 2006 •  Flux2-10 keV ≥ 1.510-11 erg s-1 cm-2 •  22 sources • 44 XMM-Newton EPIC-pn observation > 30 ks ~ 3.2 Ms of data

6. The 3-10 keV continuum Total rms “model independent” ~ fourier resolved spectroscopy Revnivtsev et al. 1999; Papadakis et al. 2005; 2007 Arevalo et al. 2008 Total rms > mean spectrum mean spectrum increases with flux Zdziarski et al. 1999; 2003; Markowitz et al. 2001

7. The 3-10 keV continuum Variable partial covering - Absorption : Boller et al. 2002; Reeves et al. 2004; Done et al. 2007; Miller et al. 2008 pc=0 nH = 1024 cm-2 Log() = 1.9 Pivoting power law : Pivot point at 20 keV pc=0.97 Trms - random shape Trms - correlated with flux

8. The 3-10 keV continuum Variable partial covering - Absorption : Boller et al. 2002; Reeves et al. 2004; Done et al. 2007; Miller et al. 2008 pc=0 nH = 1024 cm-2 Log() = 1.9 Pivoting power law : Pivot point at 20 keV pc=0.97 Trms - random shape Trms - correlated with flux Pivoting power law : Haardt et al. 1993; 1997; Poutanen et al. 1999; Zdziarski et al. 2003 =2.5 =1.7 Trms - power law Trms - correlated with flux

9. The 3-10 keV continuum Variable partial covering - Absorption : Boller et al. 2002; Reeves et al. 2004; Done et al. 2007; Miller et al. 2008 pc=0 nH = 1024 cm-2 Log() = 1.9 Pivoting power law : Pivot point at 20 keV pc=0.97 Trms - random shape Trms - correlated with flux Two components - Reflection: Pivoting power law : •  = Trms • Trms-mean=0.34 • R ~ 3 (R=1 =0.1-0.15) Haardt et al. 1993; 1997; Poutanen et al. 1999; Zdziarski et al. 2003 =2.5 =1.7 Trms -power law Trms - constant with flux Trms - power law Trms - correlated with flux McHardy et al. 1998; Shih et al. 2002; Fabian et al. 2002

10. The 3-10 keV continuum: flux dependence

11. The 3-10 keV continuum: flux dependence

12. The 3-10 keV continuum: flux dependence Papadakis et al. 2007; Gilfanov et al. 2000; Revnivtev et al. 1999; The major variability  steep (~1.8-2.6) power law varying mainly in normalisation

13. The 3-10 keV continuum: Variable Absorption NGC1365 - obs 2004 nH=1.71.4*1023 cm-22 =3.50.3 + Ionised absorption 2/dof =2.5 Papadakis et al. 2007; Gilfanov et al. 2000; Revnivtev et al. 1999;

14. Detailed study of the line variability:The case of NGC 3783 • i) FeKα+β (EW∼110±8 eV); • ii) Fe XXVI (EW∼17±5 eV); • iii) Absorption at 6.67 (EW=17±5 eV); • FeXXV; • iv) Excessredward of FeKα; • diskline (EW∼58±12 eV) • absorption + Compton shoulder FeKα+β  constant Fe XXVI emission  constant Absorption FeXXV  constant ∆χ2=28.1 for 2 dof EW=7925 eV ∆χ2=8.8 for 2 dof EW=6033 eV

15. Detailed study of the line variability:The case of NGC 3783 • i) FeKα+β (EW∼110±8 eV); • ii) Fe XXVI (EW∼17±5 eV); • iii) Absorption at 6.67 (EW=17±5 eV); • FeXXV; • iv) Excessredward of FeKα; • diskline (EW∼58±12 eV) • absorption + Compton shoulder FeKα+β  constant Fe XXVI emission  constant Absorption FeXXV  constant • Excess variable! (prob. 99.9 %) • broad line from the disk • absorption + Compton shoulder excluded! ∆χ2=28.1 for 2 dof EW=7925 eV ∆χ2=8.8 for 2 dof EW=6033 eV ∆χ2=16.7 for 2 dof same parameters! ∆χ2=11.1 for 2 dof EW=9045 eV  prob.99.9 % Tombesi et al. 2008; Talk by De Marco

16. The Fe K line: broad component

17. Sample variability over time: Sgr A* has been the brightest AGN of the sky? Galactic plane from above • Sgr A* sits on the centre of the • Central Molecular Zone (CMZ) • MC are mirrors of the GC past activity •  Tool to study history of GC emission Sgr A* d r nH Toward the Earth Sunyaev et al. 1993; 1998

18. The bridge

19. The bridge Bridge 1 11,3 

20. The bridge Bridge 1 9,1  Bridge 2

21. The bridge Bridge 1 Bridge 2 8,6  Bridge 3

22. Super-luminal motion?

23. Super-luminal motion? • Regions causally disconnected!! • No propagation of single event • Cosmic ray - internal source excluded! • Many un-correlated variations • Similar variation - distant source • L15pc~1.31038 erg s-1 - Binary in peculiar position close to bridge •  Flare Sgr A* (Sunyaev & Churazov 1998)

24. Summary: • 3-10 keV CONTINUUM: • The 3-10 keV Total rms spectrum  PL shape, without signatures of partial covering absorption • A constant ionized partial covering or variations such as in NGC1365 are excluded • total rms is the same in sources where partial covering may/is-not present • Main spectral variations due to PL varying in normalisation • Fe K BAND VARIABILITY: • 8 sourcesthe statistics/variability allows to probe the variability of the Fe K band (~20-40 eV) • In all the 8 cases the variability behaviour confirm the presence of broad Fe K lines • - In NGC 3783, NGC 4051, IC4329A the broad line is variable and correlated with continuum • in NGC 3516, MCG-5-23-16 the broad line is constant • - in Mrk 766 the red wing of the broad is constant, the blue peak variable • The red tail of the Fe K line of MCG-6-30-15 shows a significant excess of variability in one over 4 XMM-Newton observations • X-RAY EMISSION FROM MOLECULAR CLOUDS AROUND SGR A* • Sgr A* (in the recent past) was one the brightest AGN of the sky!