THE INVERSE-COMPTON X-RAY SIGNATURE OF AGN FEEDBACK

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1 THE INVERSE-COMPTON X-RAY SIGNATURE OF AGN FEEDBACK MARTIN BOURNE IN COLLABORATION WITH: SERGEI NAYAKSHIN WITH THANKS TO: ANDREW KING, KEN POUNDS, SERGEY SAZONOV AND KASTYTIS ZUBOVAS Black hole (g)astronomy Brindisi 203

2 Ultrafast outflows & the AGN-Host connection Accretion at Eddington rate believed to produce powerful winds (Shakura & Sunyaev 973; King 2003; Proga 2003). A high velocity outflow from PG Table. Parameters of the model fit to the stacked pn and MOS data from the 200, 2004 and 2007 XMM-Newton observation of PG2+43. Power law indices Γ and Γ2 refer to the primary and secondary continuum components, respectively. High and moderate ionisation absorbers affect the primary continuum, with equivalent hydrogen column densities in units of 022 cm 2 and ionisation parameters in erg cm s. The soft secondary continuum is affected only by the high ionisation absorber. Apparent redshifts are converted to ionised gas outflow velocities in the text Γ Γ2 NH logξ redshift NH logξ redshift χ2 /dof pn 2.09± ± ± ± ± ± /478 MOS 2.03± ± ± ± ± ± /354 ratio.5 ratio.5 redshift of PG2+43. A best-fit continuum was found for power law indices of Γ=2.2 and 2.9, with a cold absorbing column of 023 cm 2. Tests showed these parameters are important in determining the details of the PCygni profile deconvolution, mainly in the deduced line strengths, but do not change the need for two dominant components, one in absorption at 7 kev and a broader emission component at a lower energy. We initially analysed the PCygni line profile by adding a sequence of positive and negative Gaussians to produce a (from and Arizona.edu, fromfit.eso/wfi MPIfR/ESO/APEX/ visual quantitative The main(op;tical) profile was found to be fitted by(sugmillimeter)), the addition of NASA/CXC/CfA/R. just 2 lines, both broader A. well Weiss et al. Kraft et al. (Chandra X-ray Observatory than the resolution of the pn camera. Figure 7 shows (X-ray) and SSC/JPL-Caltech/ J. Keene (infrared)) this web site.) fit, with emission and absorption component energies (ad justed to the redshift of PG2+43) of 6.5±0.04 kev and observed energy (kev) 7.65±0.05 kev, and sigma line widths (which here include Figure 7. Double Gaussian line fit to the stacked pn data Fe K 65 ev for the pn resolution) of 20±50 ev and 70±50 ev, profile showing a classical P Cygni profile respectively. The statistical improvement by adding these 2 Gaussians is listed, together with the individual component parameters, in Table 2. Although already a good fit, the emission component in figure 7 has an obvious high data point which lies close to 5.92 kev, which corresponds (at the redshift of PG2+43) to the 6.4 kev Fe Kα line, often seen in the spectra of AGN and attributed to fluorescence from low velocity (distant?) cold matter. Adding a third Gaussian to the profile fit, with width constrained to the pn energy resolution, gave a further small but significant improvement to the fit, while increasing the energy of the broad emission component to 6.6±0.08 kev and its width to 260±60 ev. The absorption line parameters were essentially unchanged. Figure 8 reproduces this 3-Gaussian fit with parameters summarised in Table 2. The broad emission component is now consistent with observed energy (kev) the resonance s-2p transition in He-like FeXXV, the same transition as identified in the absorption spectrum in the Figure 8. Figure 7 with an additional narrow emission line at 200 data (Pounds and Page 2006). Allowing for the pn camthe rest energy of Fe K-α era resolution, an intrinsic emission line width of 250±60 ev, or 28000±7000 km s (FWHM) when interpreted solely in terms of velocity broadening, corresponds to a wide angle greater broadening of the emission line with respect to the ultra-fast outflows (UFOs) vout 0.03c 0.3c, detected via X-ray line absorption (e.g., Pounds et al. 2003a,b, Tombesi et al., 200a,b) UFOs carry enough energy to clear out significant fractions of all gas from the parent galaxy (Silk & Rees 998; King 2005; Zubovas & King 202).

3 with same n the cam0 ev, ely in angle umpcome alent ce for observed energy (kev) 8 9 Figure 7. Double Gaussian line fit to the stacked pn data Fe K profile showing a classical P Cygni profile Accretion at Eddington rate believed to produce powerful winds (Shakura & Sunyaev 973; King 2003; Proga 2003)..5 Pounds & Reeves, 2009 ultra-fast outflows (UFOs) vout 0.03c 0.3c, detected via X-ray line absorption (e.g., Pounds et al. 2003a,b, Tombesi et al., 200a,b) onent h lies ift of n the w veo the esoluo the comthe. Figsum- 4 Ultrafast outflows & the AGN-Host connection ratio dding uce a nd to oader s this (adv and clude 0 ev, ese 2 onent observed energy (kev) 8 9 Figure 8. Figure 7 with an additional narrow emission line at the rest energy of Fe K-α greater broadening of the emission line with respect to the absorption line in the stacked data is most likely due to the spread of projected velocities in a wide angle flow. To check the robustness of the broad ionised emission line in the stacked data, an alternative fit was tried with 3 narrow lines corresponding to neutral Fe K-α (rest energy UFOs carry enough energy to clear out significant fractions of all gas from the parent galaxy (Silk & Rees 998; King 2005; Zubovas & King 202).

4 Ultrafast outflows & the AGN-Host connection Accretion at Eddington rate believed to produce powerful winds (Shakura & Sunyaev 973; King 2003; Proga 2003). A high velocity outflow from PG Table. Parameters of the model fit to the stacked pn and MOS data from the 200, 2004 and 2007 XMM-Newton observation of PG2+43. Power law indices Γ and Γ2 refer to the primary and secondary continuum components, respectively. High and moderate ionisation absorbers affect the primary continuum, with equivalent hydrogen column densities in units of 022 cm 2 and ionisation parameters in erg cm s. The soft secondary continuum is affected only by the high ionisation absorber. Apparent redshifts are converted to ionised gas outflow velocities in the text Γ2 NH logξ redshift NH logξ redshift χ2 /dof 2.09± ± ± ± ± ± /478 MOS 2.03± ± ± ± ± ± /354 ratio Gültekin, K. et al. (2009b) observed energy (kev) 8 9 ratio.5 Figure 7. Double Gaussian line fit to the stacked pn data Fe K profile showing a classical P Cygni profile redshift of PG2+43. A best-fit continuum was found for power law indices of Γ=2.2 and 2.9, with a cold absorbing column of 023 cm 2. Tests showed these parameters are important in determining the details of the PCygni profile deconvolution, mainly in the deduced line strengths, but do not change the need for two dominant components, one in absorption at 7 kev and a broader emission component at a lower energy. We initially analysed the PCygni line profile by adding a sequence of positive and negative Gaussians to produce a visual and quantitative fit. The main profile was found to be well fitted by the addition of just 2 lines, both broader than the resolution of the pn camera. Figure 7 shows this fit, with emission and absorption component energies (adjusted to the redshift of PG2+43) of 6.5±0.04 kev and 7.65±0.05 kev, and sigma line widths (which here include 65 ev for the pn resolution) of 20±50 ev and 70±50 ev, respectively. The statistical improvement by adding these 2 Gaussians is listed, together with the individual component parameters, in Table 2. Although already a good fit, the emission component in figure 7 has an obvious high data point which lies close to 5.92 kev, which corresponds (at the redshift of PG2+43) to the 6.4 kev Fe Kα line, often seen in the spectra of AGN and attributed to fluorescence from low velocity (distant?) cold matter. Adding a third Gaussian to the profile fit, with width constrained to the pn energy resolution, gave a further small but significant improvement to the fit, while increasing the energy of the broad emission component to 6.6±0.08 kev and its width to 260±60 ev. The absorption line parameters were essentially unchanged. Figure 8 reproduces this 3-Gaussian fit with parameters summarised in Table 2. The broad emission component is now consistent with the resonance s-2p transition in He-like FeXXV, the same transition as identified in the absorption spectrum in the 200 data (Pounds and Page 2006). Allowing for the pn camera resolution, an intrinsic emission line width of 250±60 ev, or 28000±7000 km s (FWHM) when interpreted solely in terms of velocity broadening, corresponds to a wide angle.5 Γ pn observed energy (kev) 8 9 Figure 8. Figure 7 with an additional narrow emission line at the rest energy of Fe K-α greater broadening of the emission line with respect to the ultra-fast outflows (UFOs) vout 0.03c 0.3c, detected via X-ray line absorption (e.g., Pounds et al. 2003a,b, Tombesi et al., 200a,b) UFOs carry enough energy to clear out significant fractions of all gas from the parent galaxy (Silk & Rees 998; King 2005; Zubovas & King 202).

5 Ultra Fast Outflow schematic Wind P = M v = L Edd out w c E = 2 M out v w 2 = η L Edd 2

6 Ultra Fast Outflow schematic Shock k B T sh = 3 6 m 2 pv out P = M v = L Edd out w c E = 2 M out v w 2 = η L Edd 2

7 Inverse-Compton Up-scattered X-ray photons UV photons du dt «IC = 4 Z 3 σ TcU `γ2 rad n(γ, θ)dγ

8 Momentum or Energy driven? du dt «IC = 4 3 σ TcU rad Z `γ2 n(γ, θ)dγ U rad = L Edd 4 R 2 c at and is the t IC <t flow radiates kinetic energy momentum driven t IC >t flow retains kinetic energy energy driven d so R IC km/s M 0 8 M /2 kpc. Zubovas & King, 202

9 T vs. 2T Models T sh = 3 6 m v 2 j out ~ k B " $ # %$ K 0 7 K ions electrons Coulomb scattering Is it safe to assume a one-temperature (T) model? UFOs may be in 2T regime - Faucher-Giguere & Quataert (202) 2T regime R IC, 2T << R IC, T ~ always in energy driven regime

10 Calculating the SED Construct SED by calculating L E : dl de f = E f 2T case T case Z d df ( ) d 0 ell-jüttner distribution, df ( ) d = n(, ) = Z θsh 2 K 2 e, = ( ), is the dimensionle df (γ) = n(γ, θ) dn dγ dθ dθ θ ic Z de 0 c dn 0 d (E f,e 0, ) de 0 de f (20)

11 T - Electron energy distribution x0 0 ( -)df( )/d x0 - x0-2 x0-3 x0-4 x0-3 x0-2 x0 - x0 0 x0 x0 2 - (Bourne & Nayakshin, submitted)

12 SED v out = 0.c 0 45 Input spectrum type- Sazonov et. al 2004 v out =0.c (T regime) T e, max =2x0 9 K (2T regime) Input spectrum modeled by blackbody with k B T=3eV E dl/de (erg s - ) Assume all K.E. into emitted luminosity 2T emission likely to have lower L Energy (KeV) (Bourne & Nayakshin, submitted)

13 SED different v out E dl/de (erg s - ) Input spectrum type- Sazonov et. al 2004 type-2 Sazonov et. al 2004 v out =0.05c (T regime) v out =0.c (T regime) v out =0.2c (T regime) Input spectrum modeled by obs Type AGN, -00 ev If R shock > R torus still expect to observe spectra at low energies in Type 2 AGN Variability light crossing time t = R c ~ 30 " R % $ ' yrs # 0pc & Energy (KeV) (Bourne & Nayakshin, submitted)

14 Scattering all of the AGN emission 0 45 Input spectrum type-2 Sazonov et. al 2004 v out =0.c (T regime) T e, max =2x0 9 K (2T regime) Input spectrum modeled by obs Type AGN, -0 5 ev E dl/de (erg s - ) T emission not observed? 2T regime hard to detect? NGC 405 Pounds & Vaughan, Energy (KeV) (Bourne & Nayakshin, submitted)

15 Implications 2T regime R IC2T << R ICT Nearly always in energy conserving phase Lower mass SMBHs can clear out a galaxy? SMBHs would not reach M-σ relation BUT models assume homogeneous medium, what about a clumpy medium?

16 Implications 2T regime R IC2T << R ICT Nearly always in energy conserving phase Lower mass SMBHs can clear out a galaxy? SMBHs would not reach M-σ relation BUT models assume homogeneous medium, what about a clumpy medium?

17 Implications 2T regime R IC2T << R ICT Nearly always in energy conserving phase Lower mass SMBHs can clear out a galaxy? SMBHs would not reach M-σ relation BUT models assume homogeneous medium, what about a clumpy medium?

18 Summary Shocked outflows may have a 2T structure Whether shocks have T or 2T structure is vital in determining whether a shock is momentum or energy driven Outflows with a T structure should produce a broad SED in X-rays we believe this is not observed 2T structure leads to narrow feature in soft X-rays NGC 405 Now working on simulations of feedback on a nonhomogeneous medium

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