1. Credit goes to: M. Dadina, G. Ponti, F. Tombesi, M.Giustini, G. Palumbo (INAF+Univ. Bologna); G. Matt, S. Bianchi (Roma3) Massimo Cappi INAF-IASF, Sezione di Bologna Outflows and winds in AGNs: the case for Simbol-X 1.Framework Outflows/winds 2.X-ray Observations: latest results Blue-shifted abs. lines… 3.Current Interpretations Outflows/winds… 4.Critical Issues Significance, Identifications… 5.Importance Astrophysics, cosmology… 6.Future Simbol-X simulations… Outline Kato et al. 2003

2. …known/seen in AGNs since long ago M87 - Jet Jets in radio-loud AGNs Framework (i/ii): Fast winds/outflows/ejecta in AGNs Tadhunter & Tsvetanov, Nature, 1989; Wilson & Tsvetanov, 1994 Cappi et al. 1995 Wide-angle winds & jets in Seyfert galaxies Sey2 NGC5252 OIII cones Fast (v up to ~ 50000 km/s) winds in BAL QSOs (~ 20% of all QSOs) Weymann et al., ’91; Reichards et al., ‘03

3. 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 Framework (ii/ii): Warm absorbers…probe highest-v gas

4. X-ray Observations (i/iii): 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

5. APM 08279+5255 (z=3.91) v~0.2-0.4c 2 high-z BAL QSOs Chartas et al. 2002, Hasinger, Schartel & Komossa 2002 N.B.: Would have been undetected at z=0... Massive outflows…also (mostly?) at high redshift X-ray Observations (ii/iii): Blue-shifted absorption lines/edges – High-v & z See also Wang et al. ’05 (v=0.8c in qso@z=2.6) Chartas, Brandt & Gallagher, 2003 PG 1115+080 (z=1.72) v~0.1-0.3c MOS PN

6. WA variability on timescales 1000-10000s X-ray Observations (iii/iii): Blue-shifted absorption lines/edges - Variability Risaliti et al. 2005 NGC1365 Mrk 509 (long-look, 200ks) Cappi et al., in preparation Dadina et al. ‘05 Obs1 Obs2 Obs3 Variability allows to place limits on location, mass, etc. (See also Krongold et al. 2007 on NGC4051)

7. 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…

8. First unexpected “revolution” in extragal. astrophysics: not only most (all?) galaxies have SMBHs in their centers, but these correlate with bulge properties  evidence for feedback mechanism between SMBH(AGN) and its’ host galaxy? Magorrian et al. '98 Tremaine '02; Gebhardt '02...etc M bh ~ б 4 (see e.g. King and Pounds '03, Crenshaw, Kraemer & George '03, ARA&A) Importance (i/ii): Feedback in the (co?)evolution of galaxies

9. Second unexpected “revolution” in extragal. astrophysics: need preheating to recover L-T relations & cooling flows extra-heating  Energy feedback from AGNs/QSOs and groups&clusters? Lapi, Cavaliere & Menci, ‘05 Grav. scaling With SN preheating With AGN pre-heating With QSO ejection/outflows Perseus Cluster, Fabian et al. ‘05 Importance (ii/ii): Reheating of groups and clusters of galaxies

10. 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 ) N.B: Overall evidence is robust cz (km/s) Outflow v (km/s)

11. As far as the local “contamination” is concerned… Credit: Margherita Giustini  Existence of heavy, blue-shifted absorption lines is robust No relation with warm emitting gas and Nw<<1e21 cm**-2

12. Critical Issues (ii/ii): Interpretation/Theory Nw (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!

13. BECAUSE - “Physical bias” against highest ionization in/outflowing gas (detectable only with Fe) - “Detection bias” against transient features - “Observational bias” against highest-v blueshifted features (poor high-E sensitivity…cut-off at ~7 keV) WHILE X-ray absorption lines are naturally expected in models involving blobby/winds ejecta/outflows, such as those predicted by MHD simulations of accretion disks The tip of the Iceberg? Future (i/vii): In my opinion…

14. 2) Probe the outflow DYNAMICS ! i.e. measure delta v, not only v! (  require high throughput) 1) Probe the HIGHEST VELOCITIES (v > 0.3c), and thus masses/kinetic energy, in outflowing components (  require high-energy coverage) Daniel Proga, 2005 (failed disk winds) Future (ii/vii): Two main directions 1) + 2)  require highest possible throughput between 2-20 keV

15. Model with narrow emission and absorption lines: PL ( Г=1.9, F(2- 10)=10 -11 erg/cm2s, Exp.=50 ks) + 2 FeK emission lines (E 1 =5 keV, E 2 =6.4 keV, σ 1 = σ 2 =50 eV, EW 1 =EW 2 =100eV) + 4 FeK absorption lines (E 1,2,3,4 =7, 9, 12, 15 keV, σ 1,2,3,4 <50 eV, EW 1,2,3,4 =-100eV) Edges and absorption lines at E~7.1-9.0 keV (rest-frame) + v out ~ 0.1-0.5c   E observed ~ 8-14 keV !! Simulations of narrow emission and absorption lines Simulations Model: PL + 2 emission lines + 4 abs. lines ΔE abs <100 eV  Idea would be to follow the evolution of blobs ejecta N.B: Masses involved can be greater than M earth (10 27 g/ejecta) >>10 -11 g in accelerators Future (iii/vii): Simbol-X simulation (SDD+CdTe) Deceleration Acceleration

16. NGC1365 F(2-10)=10 -11 cgs Future (v/vii): S-X simulations SDD XMM EPIC pn (real) spectrum Risaliti et al. 2005 Simbol-X MPD simulation Credit:F. Tombesi (see Poster) 205 FeKα XXV FeKα XXVI FeKβ XXV FeKβ XXVI

17. Future (v/vii): S-X simulations SDD S-X capability of detecting blueshifted absorption lines Credit:F. Tombesi (see Poster) >20 sources (~Piccinotti sample) ~ few sources -50eV;100 ks -50eV;50 ks -25eV;50 ks -25eV;100 ks

18. Time-energy Map – SX simulation - NGC1365 - F(2-10)=10 -11 cgs Highest throughput up to 15 keV for time-resolved detections of abs. lines  real-time, extreme dynamics, outward accelerations!? (line ∆v/ ∆ t)....blob=test particle to probe launching regions of winds/jets Future (vi/vii): Simbol-X simulation SDD S-X Simulation Credit:F. Tombesi (see poster) Acceleration: 0.02c  0.2c Deceleration: 0.2c  0.02c

19. Edges and absorption lines at E~7.1-9.0 keV (rest-frame) + v out ~ 0.1-0.5c   E observed ~ 8-14 keV !! PDS 456 – A bright nearby quasar with a huge and complex warm absorber Simulations Future (vi/vii): Simbol-X simulation SDD

20. Summary I briefly presented the current evidence for blue-shifted absorption lines from highly ionized Fe in AGNs (both Sey and QSOs) These indicate existence of highly-ionized, high velocity, massive outflows in AGNs, BUT STILL ORDER OF MAGNITUDES UNCERTAINTIES on energy/momentum and mass involved. This topic still requires better measurements of intensity, energy and frequency/recurrency but has a great potential for the study of: launching mechanisms/characteristics of outflows/jets (mechanical energy emerging from BH), important not only for (relativistic) physics but also for link with cosmology Prospects for future progress are to: i)Confirm/secure these findings with longer XMM/Chandra observations ii)Probe highest-velocity gas with higher-energies (i.e Simbol-X) iii)Probe dynamics with lower time-scales (i.e. S-X, and then XEUS-like mission)

21. Thanks for your attention

22. Open Issue: Open Issue Hot corona Open Issue Credit: A. Mueller Framework (i/iii): The AGN paradigm and main open issues Characterise the geometry and mode of the accretion flow Characterise the geometry and velocity of the outflow/wind, and its impact on the host galaxy and cluster Jet Characterise the geometry, particle content, and velocity of the outflow/jet

23. ii) In an outflowing nuclear wind/jet (e.g. Reeves et al. ‘05) Interpretation II (i/ii): Gravitational redshift i) In a rotating absorbing corona (Ruszkowski & Fabian, ‘00) N.B: Origin in gravitational redshift require R<few Rg (Picture from Elvis ’00)

24. iv) “Aborted” jet (Ghisellini, Haardt, Matt ’03) Interpretation II (ii/ii): Inflowing wind/blobs/clumps iii) Failed disk wind (Proga et al. ‘00) N.B: If Infalling blobs/clouds  may represent suitable test-particles to probe GR under strong field Optical depth Density Temperature  > 1 out and inflow

25. Ejection/outflows: Massive outflows (ii/iii) McKernan, Yaqoob & Reynolds 2004 PDS456 PG1211+143 Cast doubts on the AGN origin of high-velocity absorption gas...because consistent with local WHIGM (N.B.: PDS456 is along Gal. Plane)

26. X-ray spectra of winds/outflows