1. Massimo Cappi INAF-IASF, Bologna Probing high velocity inflows and outflows in AGNs via time-resolved X-ray spectroscopy I) accretion (in)flows in AGNs Accretion modes/conditions + relativistic/fundamental physics ….from source-by-source analysis to large samples II) ejection (out)flows from AGNs Acceleration physics + interaction with host galaxies/cosmology ….from source-by-source analysis to large samples Outline Main collaborators: V. Braito, A. Celotti, M. Dadina, B. DeMarco, M. Giustini, K. Iwasawa, G. Miniutti, G. Palumbo, G. Ponti, J. Reeves, F. Tombesi, T. Yaqoob Credit: A. Mueller

2. Evidence of complex, narrow, redshifted FeK lines…  Origin in innermost regions of accretion disk+ blob-like structure (or inflowing blobs?) Turner et al. '02 XMM – NGC3516 Bianchi et al., 2004 Chandra – NGC3516 Guainazzi et al., 2003 Dovciak et al., 2004 XMM – ESO198-G024 I - Accretion/inflows: Redshifted Fe lines/components

3. Redshifted (component of) Fe lines DO show fast time variations, although not always with a clear interpretation! XMM - NGC3516 Iwasawa, Miniutti & Fabian, 2004 I - Accretion/inflows: …and variable Fe lines/components Can fit line maxima by three Keplerian orbits with same inclination & central mass !! XMM – Mrk766 Turner et al. 2005

4. I - Accretion/inflows: Source-by-source analysis NGC3783 Tombesi et al. 2007 IC4329a DeMarco et al. 2010b  Consistent with origin from hot spots, or spiral waves, in inner regions of accretion disk?

5. I - Accretion/inflows: From source-by-source to representative samples But see Barbara De Marco’s talk, this afternoon  Variability in redshifted Fe line on time-scales ~10 ks demonstrate its origin within few tens R g (hot spots, spiral waves, or else?? Not really clear) 

6. Fabian, et al. ’94 Otani, ’95, PhD Reynolds et al. '97 Georges et al. '97 50% of all Sey 1s exhibit WAs ASCA Many details from Chandra/XMM gratings NGC3783 Exp=900 ks Kaspi et al. '01; Netzer et al. '02; Georges et al. '03; Krongold et al. ‘03  Clear now that often multiple ionization & kinetic components: outflows with v~100-1000 km/s Blustin et al. 2004 II - Ejection/outflows: Warm absorbers…probe highest-v gas

7. II - Ejection/outflows: Blue-shifted absorption lines/edges – High-v PG1211+143 (z=0.08) v ~ 0.1c 2 Energy (keV) 5 7 10 New and unexpected results from Chandra and XMM-Newton observations Pounds et al. 2003a,b  massive, high velocity and highly ionized outflows in several RQ AGNs/QSOs Mass outflow rate: comparable to Edd. Acc. rate (~M ◉ /yr); velocity ~0.1-0.2 c (If) interpreted as Kα resonant absorption by Fe XXV (6.70 keV) or FeXXVI (6.96 keV) Reeves et al. 2003 PDS456 (z=0.18) v ~ 0.1c 2 Energy (keV) 5 7 10

8. Absorbers variability on timescales 1000-10000s II - Ejection/outflows: Blue-shifted absorption lines/edges - Variability Risaliti et al. 2005 NGC1365 Mrk 509 (long-look, 200ks) MC et al., 2009 Dadina et al. ‘05 Obs1 Obs2 Obs3 Variability allows to place limits on location, mass, etc. (See also Krongold et al. 2007 on NGC4051)

9. MRK509 contour plots (MC et al. 2009) Mrk 509: Among brightest F~2-5x10 -11 cgs and most luminous L~1-3x10 44 ergs/s Type 1 Sey known EW(FeXXVI)~-20 -60 eV V~0.14-0.2c ∆t~100 ks Log  ~5 erg cm/s, Nh~2-4x10 23 cm -2, v~0.14-0.2c From absorber parameters and variability, we estimated: R<500 Rs MC et al. 2009

10. Again, absorber variability on timescales ~20000s MCG-5-23-16 (XMM+Chandra) Braito et al., 2007 X-ray Observations: Variability Data require large Nw, high , and v out =0.1c

11. iii) Magnetically driven winds from accretion disk Emmering, Blandford & Shlosman, ’92; Kato et al. ‘03 Interpretation: (Three main) Wind dynamical models i) Thermally driven winds from BLR or torus Balsara & Krolik, 93; Woods et al. ‘96 i)  Large R, low v ii) and iii)  Low R and large v Murray et al. ‘95, Proga et al. ‘00 ii) Radiative-driven wind from accretion disk …and/or…

12. Theoretical Interpretation: (Three main) Wind dynamical models MHD+LD model by Proga et al. ‘00, ‘03 Overall numbers (Nh, , vout, etc.) are consistent with observations…

13. Data Interpretation: Sim et al., 2008 Yes indeed…one expects (mostly/only) strong Fe line absorptions when accounting for proper wind geometries and physics

14. Critical Issues (i/ii): Observations 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 ) cz (km/s) Outflow v (km/s)

15. Critical Issues (ii/ii): Interpretation/Theory N w (cm -2 ) Location (R, DeltaR) Ionization state (  ) Velocity Covering factor Frequency in AGNs Current estimates have order of magnitude uncertainties, they go from: dM/dt (  L kin ) few % to several times dM acc /dt (  L edd ) This is a fundamental (open) issue Elvis et al. ‘00, Creenshaw et al. ’03, King et al. ‘03, Chartas et al. ‘03, Yaqoob et al. ‘05, Blustin et al. ‘05, Risaliti et al. ’05, Krongold et al. ‘07 Fundamental to: i)PHYSICS of accelerated and accreted flows (winds?, blobs?, etc.), i.e. understand how BHs accelerate earth-like quantities of gas to relativistic velocities ii)COSMOLOGY: i.e. estimate the mass outflow rate, thus the impact of AGN outflows on ISM and IGM enrichment and heating!

16. Selection of all NLSy1, Sy1 and Sy2 in RXTE All-Sky Slew Survey Catalog (XSS; Revnivtsev et al. 2004) Cross-correlation with XMM-Newton Accepted Targets Catalog 44 objects for 104 pointed XMM-Newton observations Local (z<0.1) X-ray bright (F 4-10keV =10 -12 -10 -10 erg s -1 cm -2 ) z distribution of sources 4-10keV fluxes Again, we analysed in a systematic and uniform way, a (almost) complete sample of nearby, X-ray bright, radio-quiet AGNs (Tombesi et al. 2010a) I - Ejection/outflows: From source-by-sources to representative samples…

17. Absorption lines search Uniform spectral analysis: Reduction and analysis of all EPIC pn spectra in the 4-10keV Baseline model: absorbed power-law + Gaussian Fe K emission lines Example of PG1211+143 (Tombesi et al. 2010a) Absorption lines search: Addition of narrow line to baseline model stepping energy in 4- 10keV and recording Δχ 2 deviations Visualization on energy-intensity contour plot (significance 68% red, 90% green, 99% blue) (e.g. Miniutti et al. 2007, MC et al. 2009) Selection of narrow lines with F-test confidence levels ≥99% Line parameters determined by direct fitting to the data Absorbed power-law Absorbed power-law + emission line

18. Absorption lines significance Extensive Monte Carlo simulations (e.g. MC et al. 2009) Additional significance test for lines at energies ≥7.1keV Null hypothesis that spectra are fitted by model without absorption lines 10 3 simulated spectra for each case Simulated Δχ 2 distribution for random generated lines Selection of lines with MC confidence levels ≥95% F-test can overestimate the detection significance for a blind search of emission/absorption lines over a range of energies (e.g. Protassov et al. 2002). Global probability for the lines to be generated by random fluctuations is very low (≤10 -8 from Binomial distribution). Checked no contamination from pn background and calibration Independent confirmation of blue-shifted lines detection from MOS data (without relying on any statistical method)

19. Results: Yes, we confirm there are indeed UFOs! (Ultra-Fast Outflows…) 36 absorption lines detected in all 104 XMM observations Identified with FeXXV and FeXXVI K-shell resonant absorption 19/44 objects with absorption lines (≈43%) 17/44 objects with blue-shifted absorption lines (lower limit ≈39%, can reach a maximum of ≈60%) 11/44 objects with outflow velocity >0.1c (≈25%) Blue-shift velocity distribution ~0-0.3c, peak ~0.1c Average outflow velocity 0.110±0.004 c Blue-shift velocity distributionCumulative velocity distribution Tombesi et al. 2010a (The UFO’s hunters commander in chief)

20. Results Most frequent detected line is FeXXVI Lyα EW is in the range ≈10-100eV, with mean ≈40-50eV Estimated global covering factor from fraction of sources with lines (C=Ω⁄4Π)≈0.4-0.6 Geometry not very collimated, large opening angles favored (similar to WA) Lines EW distribution

21. Last but not least…for those still skepticals on UFOs Publication bias solved : Uniform analysis on complete sample of sources Lines detection assessed by MC simulations Global chance probability very low (≤10 -8 ) Detection independently confirmed by MOS data Not due to local contamination: No correlation between cosmological red- shift and lines blue-shift, no local (z≈0) absorption.

22. Physical photo-ionization modelling using XSTAR Xstar grid for direct spectral fitting: input enenergy band 0.1eV, 10 6 eV mean SED for radio-quiet sources power-law Γ =2 for radio-loud sources turbulent velocity v=500 km/s Mean phenomenological SED from the radio-quiet sample: SEDs 34 Type 1s from NED database scattering due to source variability and different instruments normalized SEDs to near-IR inflection point ~1.25 μ m (like Elvis et al. 1994) average flux for each energy point Simple mean SED with three intervals: Radio to mm ( Γ ~2), mm to IR ( Γ ~0.1), IR to X-rays ( Γ ~2)  N H ~10 22 -10 24 cm -2, log ξ ~3-6 erg s -1 cm -2 (v out, N H lower limits, unknown inclination angle)

23. Ejection/outflows: estimated distances r<0.01-0.1pc (<10 2 -10 5 r s ) (accretion disk winds? e.g. Elvis 2000; King & Pounds 2003 ) Often v out > v esc, but not always, material shall fall back sometimes? (“aborted jet”? e.g. Ghisellini et al. 2004, Dadina et al. 2005) variability time scales t~1day – 1year L bol /L Edd ~0.1-1 M out /M acc ~0.1-1 E k ~10 44 -10 45 erg s -1 ~0.1 L bol (last two estimates depend on covering fraction C) Acceleration mechanism? Line, magnetically or momentum driven?

24. WAs in RQ from McKernan et al. (2007) (filled black circles), WA in RL from Torresi et al. (2009) and Reeves et al. (2009) (filled blue triangle), UFOs in RQ (red crosses)

25. Ejection/outflows: Momentum-driven accretion disk winds/outflows? As in King 2009? “Eddington winds from AGN are likely to have velocities ~0.1c and show the presence of helium- or hydrogen-like iron” (King 2009) Eddington accretion episodes L bol /L Edd ~0.1-1 electron scattering wind τ ~1 at infinity wind momentuum ~ photon momentuum (M out v~L Edd /c) typical velocity ~0.1c typical ionization parameter log ξ ~4 and linear relation v out and ξ (Fe XXV, Fe XXVI + Nickel ions?) wind interaction with host galaxy, ram pressure important for feedback SMBH and host galaxy does explain the M- σ relation

26. Future prospects: Astro-H calorimeter Calorimeter on board Astro-H, next Japanese X-ray satellite to be launched in 2013: good effective area (≈250 cm 2 @ 6keV) and high energy resolution (FWHM≈7eV) from 0.1keV up to 12-13keV. realistic spectra simulations of UFOs absorption lines resolved, measured velocity broadening (down to ~100-200 km/s @ 6 keV) estimates EW, blue-shift, centroid energies ~10 times better XIS-FI (100ks simulation) better constrains on N H, logξ, v turbu

27. Future pospects: IXO calorimeter X-ray Microcalorimeter Spectrometer (XMS): high effective area ~0.65m 2 (~6500cm 2 !!) @ 6keV and high energy resolution (FWHM≈2.5eV) from 0.1keV up to 12-13keV. Flux limits 2-10keV flux limits for 5σ detection of narrow absorption lines in the 3-11keV Different EWs, exposure times and responses Lines of EW=10eV (50eV) in ≈6-9keV for ≈10 -12 (10 -13 ) erg s -1 cm -2 (expo 100ks) Spectral variability on time-scales of 5 (10) ks for ≈10 -11 (10 -12 ) erg s -1 cm -2 Flux limits (EW=10eV) (Tombesi et al. 2009)log ξ =3 erg s -1 cm, N H =10 23 cm -2, b=1000km/s (Tombesi et al. 2009) Spectra simulations Simulations of highly ionized and massive absorbers FeXXV/XXVI K lines detectable with high significance Line details (profile, energy, broadening) measured with high accuracy (>30 times Astro-H) Extend study to less bright sources Time variability, dynamics of absorbers

28. Summary I) accretion (in)flows in AGNs Redshifted FeK lines/components do vary on short time-scales Probe of accretion modes/conditions + relativistic/fundamental physics II) ejection (out)flows from AGNs Blueshifted Fe absorption lines confirmed, and variable Probe launching regions of winds/jets + Impact for feedback After 10 years of Chandra and XMM-Newton observations, we are able to move from source-by-source analysis to representative samples:

29. IXO Science Case for YB in CV- Call for ideas/contributions/suggestions Section on Strong Gravity: (<7 pages) The idea is to start from white papers + RFI1&2 for Decadal, and UPDATE with new results I- Probing Strong Gravity with X-rays: Time-resolved spectroscopy to probe the kinematics and dynamics of the inner BLR and wind/jet formation regions Time-resolved spectroscopy (e.g. waterfalling diagram) to probe the kinematics and dynamics of the inner regions of accretion disk....the idea could be to present these studies as unique way to probe/go/travel from the outer parts down into the innermost regions of the accretion disk (where winds/blobs/ejecta/jets also form). II- Measuring BH Spins with X-rays, using several independent techniques: FeK+FeL fitting, and time-lags Continuum fitting (in GBHCs and AGNs) QPOs time-resolved spcetroscopy (i.e. reverberation) Polarization measurements...the idea would/could be to present the 5 different (independent!) techniques as a way to then "calibrate" the FeK measurements, that is the technique we want to be able to apply to several tens of AGNs (maybe up to z about 1) in order to attempt the "spin distributions" Contact me directly (cappi@iasfbo.inaf.it) for any contributionscappi@iasfbo.inaf.it Any other section (i.e. Neutron Stars) or Observatory Science: Call for ideas/proposals from Xavier Barcons Due date is end of April

30. Thanks for your attention, and by the way, watch-out for UFOs!

31. II- X-ray absorption spectroscopy: Probe of launching regions of winds/jets/UFOs Credit: A. Mueller After 10 years of Chandra and XMM-Newton observations, we are able to move from source-by-source analysis to representative samples I - X-ray emission spectroscopy: Probe of innermost regions of accretion disk Jet

32. III– Complex Absorption FeK lines: Narrow/broad(?) redshifted absorption lines: Accretion/inflows: A parenthesis….  Direct probe of relativistic bulk inflows! (v~0.1-0.3c) MCG-6-30-15 in low state (Ponti, private com.) (Longinotti et al., submitted to A&A.) i) Fake lines? ii) (very) wrong continuum (WA)? iii) 2 different lines?  1 narrow + 1 Kerr (red, reverberation, tail of a Kerr line ?) iv) 1 relativistic line with resonant absorption? Mrk335 E1821+643 (z=0.3) HETG data (Yaqoob & Serlemitsos, 2005) (Reeves et al., astro-ph/0509280) PG1211+143 (z=0.08) Chandra data VERY NEW! and much debated Mrk 509 and 3516, nandra and dadina