Probing variable iron emission and absorption lines in AGNs with XEUS. Massimo Cappi. IASF-Bologna

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1 Probing variable iron emission and absorption lines in AGNs with XEUS Massimo Cappi INAF/IASF-Bologna IASF-Bologna Outline 1. Evidence for (redshifted) relativistic Fe emission lines 2. Evidence for VARIABLE Fe emission lines 3. Evidence for (blueshifted) relativistic ABSORPTION Fe lines 4. Evidence for VARIABLE Fe absorption lines 5. Future with/for XEUS Kato et al With help from Mauro Dadina, Barbara DeMarco, Magherita Giustini, Annalia Longinotti, Gabriele Ponti, Francesco Tombesi

2 X-raying the innermost regions of accretion and ejection flows Jet X-ray absorption spectroscopy: Probe of launching regions of jets/winds X-ray reflection spectroscopy: Probe of innermost regions of accretion disk Credit: A. Mueller Hot X-ray emitting corona Goals are to characterise the accretion and ejection flows near SMBHs

3 Accretion (i/i): Evidence for relativistic Fe emission lines I Broad, redshifted or double-peaked FeK lines: often weak, but quite common (~2/3 rd ) EW(Broad FeK) ev main types of broad lines: -Redshifted broad diskline (EW~ ev ev) See Fabian s talk See poster by Longinotti et al. (FERO project) -Double-peaked profile Dovciak et al., 04 (EW<60 ev) Confirms results from Nandra et al. 07, MNRAS, 382, 194 (N.B: See also many results showed at ESAC s wokshop on broad lines AN, 2006)

4 Accretion (i/iv): Evidence for variable Fe emission lines model independent evidence that lines are indeed relativistic XMM - MCG MCG Clean flare RMS variability (%) Ponti et al., 2004, Variability of redshifted Fe component on short time-scales (~ 1000s) model-independent evidence that line originates in innermost regions of accretion disk

5 Accretion (ii/iv): Evidence for variable Fe emission lines Statistics are a bit more complex, but key point is that Fe lines DO show fast time variations and redshifted energies!! XMM NGC3783 XMM - NGC3516 Iwasawa et al., 2004 Tombesi et al., 2007 Origin from orbiting hot spots in innermost regions of accretion disk?

6 Accretion (iii/iv): Evidence for variable Fe emission lines Orbital period (23 ks) + diskline fit of the line r about 9-15 Rg, consistent with a hot spot or a spiral wave (Tombesi et al. 2007) (Armitage & Reynolds 2003)

7 Accretion (iv/iv): Evidence for variable Fe emission lines T about 32 ks, d about 20 rg, time-lag 15 ks, De Marco et al., 2008, submitted

8 Ejection (i/ii): Evidence for blue-shifted absorption Fe lines (High-v) PG (z=0.08) v~0.1c 2 Energy (kev) Pounds et al. 2003a,b PDS456 (z=0.18) v~0.1c (If) interpreted as Kα resonant absorption by Fe XXV (6.70 kev) or FeXXVI (6.96 kev) 2 Energy (kev) Reeves et al massive, high velocity and highly ionized outflows in several RQ AGNs/QSOs Mass outflow rate: comparable to Edd. Acc. rate (~M /yr); velocity ~ c

9 Ejection (ii/ii): Evidence for blue-shifted absorption Fe lines (High-z) Massive outflows also (mostly?) at high redshift 2 high-z BAL QSOs PG (z=1.72) v~ c Chartas et al. 2002, Hasinger, Schartel & Komossa 2002 APM (z=3.91) v~ c MOS PN Chartas, Brandt & Gallagher, 2003 N.B.: Would have been undetected at z=0... See also Wang et al. 05 (v=0.8c in qso@z=2.6) and review by Cappi 2006, AN

10 Ejection (ii/ii): Evidence for blue-shifted absorption Fe lines NGC1365 WA variability on timescales s Mrk 509 (long-look, 200ks) Obs1 Obs2 Obs3 Risaliti et al (See also Krongold et al. 2007) Cappi et al., in preparation Dadina et al. 05 Different phases in WA shall respond differently in time

11 Future (i/vi): I see two main directions Daniel Proga, 2005 (failed disk winds) 1) Probe the flow DYNAMICS! (i.e. accelerations in innermost regions, near BHs) - Measure delta v, not only v! - On short time-scales (less than few 1000s) 2) Probe the HIGHEST VELOCITIES (v > 0.3c), and thus masses/kinetic energy, in outflowing components

12 Future (ii/vi): Reduce timescales to probe the flow dynamics ( v/ t) of innermost regions by means of detection and time-resolved spectroscopy of energy-shifted absorption lines. Fiducial numbers: We wish to follow emission and absorption lines from, say, ~1 to ~10 Rs, with intervals of 1Rs Let assume v~0.2c, then for BH mass= 10 8 M Time-scale ~ 5000 s BH mass= 10 6 M ΔTime-scale ~ 50 s (Note: 1µs if 1 M ) Scaling from Mrk509 and XMM, and assuming EW(Fe)=50 ev Con-X(6000cm 2 ) F(2-10)=2x10-11 cgs (~ 15 sources) 1000s 100s F(2-10)=2x10-12 cgs (~ 50 sources) 10000s 1000s F(2-10)=2x10-13 cgs (~ 250 sources) s 10000s N.B.: If v>0.2c, timescales consequently reduced XEUS(25000cm 2 )@6keV Really needed because mostly BH mass 10 7 M

13 Area kev XEUS XEUS x3 x4 CON-X XMM(PN) Con-X x15 x10 XMM (pn) A large effective area at energies E>3 kev is the major observational requirement for Fe emission and absorption X-ray spectroscopy

14 Future (iii/vi): XEUS simulation TES (2 m kev) Mrk509: XEUS TES F(2-10)=10-11 cgs Exposure=100s S/N>3 V=±0.1c Simulations V=±0.2c V=±0.3c

15 Future (iv/vi): XEUS simulations WFI (2.5 m kev) NGC1365 F(2-10)=10-11 cgs S/N>3 XMM results Risaliti et al XEUS Simulation

16 Future (v/vi): XEUS simulations WFI (2.5 m kev) NGC1365 F(2-10)=10-11 cgs S/N>3 Accelerated flow Decelerated flow Simulation Credit:F. Tombesi Highest throughput for time-resolved detections of abs./em. lines real-time, extreme dynamics, i.e. inward and outward accelerations!? (line v/ t)...blob=test particle to test Kerr vs. Schwarzschild GR

17 Future (vi/vi): As shown by Andy yesterday, the ultimate goal is. Armitage and Reynolds 2003

18 Conclusions Clear evidence for relativistic emission and absorption Fe lines Clear evidence for variable, often transient, emission and absorption lines Variability on (short) time-scales equivalent to a few gravitational radii Demonstrate Fe lines produced in the innermost regions of accretion disk (emission) and launching regions of jets/winds (absorption) And this is a model-independent evidence Likely tip of the iceberg points to the need for: 1 ) Very high (>2m kev) throughput (main req.) 2) High 6 kev and high-e (E>10 kev) coverage (second req.)

19 Thanks for your attention

20 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 Outflow v (km/s) cz (km/s)

21 Future (i/vii): In my opinion The tip of the Iceberg? 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

22 Future (vii/vii): XEUS simulation (with CdTe) PDS456: XEUS WFI + CdTe (100 ks exposure) v=0.1c Simulations v=0.5c (?) (Wfi: S/N=100; Cdte: S/N=10) (Wfi: S/N=50; Cdte: S/N=10) Edges at E~ kev (rest-frame) + v out ~ c E observed ~ 8-14 kev!! (maybe the reason why never seen earlier, except for high-z sources) High energies is a MUST HAVE to study relativistic outflows

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

24 Importance (i/ii): Feedback in the (co?)evolution of galaxies 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? See Talks by Page and Croston Magorrian et al. '98 M Tremaine '02; Gebhardt '02...etc bh ~ б 4 (see e.g. King and Pounds '03, Crenshaw, Kraemer & George '03, ARA&A)

25 Importance (ii/ii): Reheating of groups and clusters of galaxies 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? Grav. scaling With SN preheating With AGN pre-heating With QSO ejection/outflows See Talk by Sanders Lapi, Cavaliere & Menci, 05 Perseus Cluster, Fabian et al. 05

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

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

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

29 Ejection/outflows: Massive outflows (iii/iii) Credit: M. Giustini

30 X-ray spectra of winds/outflows

31 Framework (iv/iv): Warm absorbers variable Mrk766 RGS WA variability on timescales s Mrk766 EPIC pn (RMS) RMS variability (%) Mason et al Ponti et al., PhD thesis Different phases in WA shall respond differently: e.g. with a range of response times in a radially segregated flow. This will be crucial to determine location and covering factor

32 Accretion/inflows: Observations (8/8) Post-Chandra & XMM-Newton III Complex Absorption FeK lines: Narrow/broad(?) redshifted absorption lines: Mrk335 VERY NEW! and much debated MCG in low state (Ponti, private com.) (Longinotti et al., submitted to A&A.) PG (z=0.08) Chandra data (Reeves et al., astro-ph/ ) E (z=0.3) HETG data (Yaqoob & Serlemitsos, 2005) i) Fake lines? ii) (very) wrong continuum (WA)? iii) 2 different lines? Þ 1 narrow + 1 Kerr (red, reverberation, tail of a Kerr line?) iv) 1 relativistic line with resonant absorption? Þ Direct probe of relativistic bulk inflows! (v~ c)

33 Future (vi/vii): Simbol-X simulation (SDD+CdTe) Simulations of narrow emission and absorption lines Model: PL + 2 emission lines + 4 abs. lines Simulations 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~ kev (rest-frame) + v out ~ c Þ E observed ~ 8-14 kev!! DE abs <100 ev Þ Idee would be to follow the evolution of blob ejections (or injections) N.B: Masses involved can be greater than M earth (10 27 g/ejecta) >>10-11 g in accelerators Deceleration Acceleration

34 Not only winds and accretion disk, but also outflowing and inflowing clouds? Blueshifted Lines? Inverse P-Cygni profile if wind? Gauss. abs. line if blobs? Redshifte d Lines? Quasar wind model by Elvis 2000 v/c= Magnetic Tower by Kato et al (see also Lynden-Bell 2003)

35 Unfortunately XRS on-board ASTRO-E2 is lost Mrk 509, Astro-E2 simulation 100 ks Simulations High energy resolution to distinguish beetwen wind and blob(s) (line profile)

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