Nuclear X-ray Emission and Mass Outflow From Broad Lined Radio Galaxies (Lorentz Center, Leiden 2009) James Reeves (Keele Univ, UK) Collaborators:- Rita Sambruna (NASA/GSFC), Francesco Tombesi (NASA/GSFC & Bologna), Valentina Braito (Leicester), Lucia Ballo (Santander), Jason Gofford (Keele)
AGN have powerful outflows Some have powerful, relativistic jets on kpc/mpc scales A Dichotomy - Radio Loud AGN have jets. Radio-quiet AGN disc winds? Do Radio-Loud AGN have radiatively driven winds as well as jets?
Highly Ionized Outflows in Radio-Quiet AGN PG 1211+143, z=0.081 (Pounds et al. 03) PDS 456, z=0.184 (Reeves et al. 03, 09) EPIC-pn XMM/EPIC-pn XMM/EPIC-MOS Blue-shifted absorption due to highly ionized iron (e.g. Fe XXV) as well as Mg/Si/S. Velocities implied are 0.1-0.2c, launched from < 100Rg, with columns >10 23 cm -2. Suggests kinetic power ~ L Edd. (see also King & Pounds 2003; King 03).
Fast, Radiatively Driven Disk Winds? Disk winds simulations of Proga (2004; 2007), recently Sim et al. (2008), Schurch et al. (2008) Can produce high ionization absorption lines at Fe Kα (e.g. PDS 456, PG 1211+143). Terminal velocities ~ 0.1-0.3c, densities (107-1010 atoms cm-3) and columns (1022-1024 cm-2) consistent with observed systems.
Suzaku Observations of BLRGs OUR PROGRAM: BLRGs at z<0.1 3C 390.3: 100 ks (Sambruna et al. 2009) + XMM 3C 382: 100 ks + 150ks Chandra/HETG (Reeves et al. 2009) 3C 445: 120 ks + 200ks Chandra/LETG 3C 111: 100 ks (Ballo et al. 2009) 3C 120: 160 ks (Kataoka et al. 2007, GTO program)
XMM/Chandra Suzaku Suzaku s Broad Bandpass Absorption from outflow Iron K Line X-ray Continuum Soft Excess Compton Reflection hump
Broad-band spectra 3C 390.3 3C 382 3C 111 3C 445 Low/Hard
Fe Kα line profiles 3C 390.3 3C 382 3C 111 3C 120
Suzaku Parameters at a Glance BLRGs: EW α ~ 50-100 ev r in ~ 9, 20 r g R cold ~ 0.2-0.6 Γ ~ 1.6-1.8 E cutoff ~ 100-200 kev Seyfert 1s: EW α ~ 40-300 ev r in ~ 2-100 r g R ~ 1 (mean) Γ~ 2.0 (mean) E cutoff ~ 50-150 X-ray continuum emision in these bright BLRGs dominated by disk emission rather than jet Suzaku is blurring the distinction RL-RQ in X-rays No longer a dichotomy but continuous distribution ---> BH spin the main agent for RLoudness?
A parsec scale wind in 3C 382 (Reeves et al. 2009) Chandra/HETGS 150 ks N H =(1.3±0.2)x10 21 cm -2 Log ξ = 2.4±0.1 (cgs) [Note here ξ = L ion /n r 2 ] v out = -840±60 km/s σ = 340 ± 70 km/s L ion = 1.2 x 10 45 erg/s Wind is coincident with NLR. Location r = 10-1000 pc. Densities n=0.4-2400 cm -3. Outflow rate M out < 100 M sol yr -1. Kinetic output de/dt < 3 x10 43 erg s -1 (<2% of ionizing luminosity). Velocity width and blueshifts consistent with O [III], O [I], Si [II] line profiles and also extended O [III] gas.
Highly Ionized Outflow in 3C 445 Chandra/LETG, 200ks Highly absorbed X-ray continuum:- N H = 7x10 23 cm -2, log xi = 2.7 v out = 5000-10000 km s -1, L ion = 3x10 44 erg s -1 Soft X-ray emission Photoionized soft X-ray emission lines (e.g. O VII, O VIII, Ne IX/X, Mg XI/XII) + Fe Kalpha Vel width (e.g. O VIII), σ=900±400 km s -1 No outflow v out <400 km/s
Outflow Parameters for 3C 445 Soft X-ray line emitting gas (except Kalpha) on extended pc scales (~5-10 pc) and no outflow required. However substantial outflowing gas seen in absorption (greater inclination angle of 3C 445?) Absorber location sub pc (r< 0.3 pc) Mass outflow rate = 10 M sun yr -1 (minimum) Equivalent to de/dt 10 44-10 45 erg/s (a significant fraction of L bol )
Highly Ionized Outflows in BLRGs (Tombesi et al. 2010) 3C 111 / Suzaku @ Fe K Systematic search for highly ionized (outflowing) absorption in Fe K band for all 5 BLRGs Absorption also present in 3C 111, 3C 120, 3C 390.3. Not detected in 3C 382. Outflow velocities 0.04c, 0.08c, 0.15c respectively. In 3C 111, absorber may be bound as v wind < v esc at estimated r wind. In 3C 390.3, 3C 120 dm out /dt = 2, 17 M sun yr -1. de/dt ~ 10 45 erg s -1 High global covering fraction - significant in terms of feedback.
No X-ray Outflow in PKS 1549-79 XMM/80ks Luminous, but obscured quasar at z=0.152 (Holt et al. 2006), accreting near Eddington. X-ray spectrum consistent with power-law absorbed by neutral absorption column only (consitent with optical reddening) No apparent X-ray lines (e.g. at Fe K) in either XMM or Suzaku spectrum. No highly ionized outflow in X- rays, unless gas is fully ionized - scattered soft emission?
Conclusions - Mass outflow in radio-loud AGN How much mass is carried out of the AGN by the outflow? In the high v outflows, launched from the inner disk (~100 Rg) mass outflow rates are at least few x solar (e.g. 3C 120, 3C 390.3, 3C 445) e.g. 3C 120, dm out / dt = 4πbm p v out L ion / ξ ~ 17b M sun yr -1. b is a geometrical global covering factor. From observations, global covering at least 40%. How does it compare to the amount of matter being accreted? For high velocity outflows in high M dot /M Edd BLRGs, a substantial fraction is driven in the outflow, i.e. dm out / dt ~ M dot
Mass outflow in radio-loud AGN Does the ionized outflow carry a significant fraction of the energy output of the AGN? Yes, for some BLRG (e.g. 3C 120, 3C 390.3, 3C 445), de out / dt ~10 45 erg/s and L out L ion Could the outflows be energetically significant in terms of feedback? If de out/ dt ~ 10 45 erg/s for lifetime of AGN phase (t >10 7 yr) then E>10 59 ergs (c.f. E=10 59 ergs of a bulge with 10 11 Msolar and σ=300 km/s, also see King 03)