1. The mass-energy budget of the ionised outflow in NGC 7469 Alexander J. Blustin STFC Postdoctoral Fellow, UCL Mullard Space Science Laboratory Chandra X-ray Gratings Meeting, Cambridge, MA, 11 th July 2007 In collaboration with G. Kriss (STSCI), T. Holczer (Technion), E. Behar (Technion), J. Kaastra (SRON), M. Page (UCL-MSSL), S. Kaspi (Tel-Aviv), G. Branduardi- Raymont (UCL-MSSL), K. Steenbrugge (Oxford)

2. ionised wind X-ray absorption – more ionised Blustin et al. 2007, 466, 107 UV absorption – less ionised Kriss, Blustin et al. 2003, A&A 403, 473 Artist’s impression of ionised wind in nuclear region of a galaxy (A. Blustin) What is the total mass-energy output through an AGN wind? How biased is this by the waveband in which we do the spectroscopy?

3. Dataset and spectral continuum NGC 7469 (z = 0.0164) is an X-ray and UV bright Seyfert with a low- column warm absorber 164 ks with XMM-Newton, obtained in Nov/Dec 2004 Highest signal-to-noise X-ray grating and CCD spectra yet obtained for this source Basic form of spectral continuum obtained from EPIC-pn: power-law (  = 1.81) plus soft excess (we used a 0.144 keV blackbody component). Significant soft X-ray residuals are visible Blustin et al. 2007, A&A 466, 107

4. The X-ray absorption and emission features Significance of narrow spectral features  2 = 16 implies 4  significance Blustin et al. 2007, A&A 466, 107

5. Fitting individual ionic columns Ion-by-ion (slab in SPEX) absorber model superimposed on RGS data Individual ion columns Blustin et al. 2007, A&A 466, 107

6. Absorption Measure Distribution (AMD) See talk by Tomer Holczer for more details on AMDs The AMD expresses the total line-of- sight column density as an integral over its distribution in log  N Htotal = (3.3 ± 0.8) x 10 21 cm -2 Two main ionisation regimes: most gas at higher levels of ionisation Blustin et al. 2007, A&A 466, 107

7. Photoionised absorber modelling Spectral Energy Distribution (SED) used to calculate SPEX xabs photoionised absorber model has PN spectral slope, and is normalised using fluxes from RGS and OM Scott et al. 2005 SED for Chandra/FUSE data Blustin et al. 2007 SED for XMM-Newton data Blustin et al. 2007, A&A 466, 107

8. Photoionised absorber modelling 3 absorber components: X-ray 1 X-ray 2 X-ray 3 Log  = 0.8 +0.4 -0.3 Log N H = 19.5 ± 0.2 cm -2 v = -2300 ± 200 km s -1 Log  = 2.73 ± 0.03 Log N H = 21.30 +0.04 -0.05 cm -2 v = -720 ± 50 km s -1 Log  = 3.56 +0.08 -0.07 Log N H = 21.5 ± 0.1 cm -2 v = -580 +80 -50 km s -1 Blustin et al. 2007, A&A 466, 107

9. Velocity components in the X-ray absorber

10. Comparison with UV-absorbing outflow Log  v (km/s) N CIV N NV N HI Ionic columns (10 14 cm -2 ) UV 11.61562 ± 60.98 ± 0.092.9 ± 0.87 ± 2 UV20.511901 ± 62.0 ± 0.12.5 ± 0.22.4 ±0.5 X-ray 10.8 +0.4 -0.3 2300 ± 2001.63.46.2 X-ray 22.73 ± 0.03720 ± 50n/a0.00091n/a X-ray 33.56 +0.08 -0.07 580 +80 -50 n/an/an/a UV properties from Scott et al. 2005

11. Comparison with UV-absorbing outflow Log  v (km/s) N CIV N NV N HI Ionic columns (10 14 cm -2 ) Identify UV component 2 with X-ray component 1 UV 11.61562 ± 60.98 ± 0.092.9 ± 0.87 ± 2 UV20.511901 ± 62.0 ± 0.12.5 ± 0.22.4 ±0.5 X-ray 10.8 +0.4 -0.3 2300 ± 2001.63.46.2 X-ray 22.73 ± 0.03720 ± 50n/a0.00091n/a X-ray 33.56 +0.08 -0.07 580 +80 -50 n/an/an/a UV properties from Scott et al. 2005

12. The location of the soft X-ray/UV absorbing outflow Outflow component Distance estimates: R min from escape velocity R max from  R/R ≤ 1 Blustin et al. 2007, A&A 466, 107

13. Calculating the mass and energy transport of the outflow Mass outflow rate, M out ~ 1.23 m proton L ion C v v  . Volume filling factor of the outflow obtained from the assumption that, for a radiatively driven wind: Momentum of outflowing matter ~ Momentum of radiation absorbed and scattered by wind Blustin et al. 2005, A&A 431, 111

14. Calculating the mass and energy transport of the outflow Mass outflow rate, M out ~ 1.23 m proton L ion C v v  . Kinetic luminosity, L KEout = M out v 2. 1 2 Volume filling factor, C v ~ 1.23 m proton c L ion v 2  (L abs + L scatt )  Blustin et al. 2005, A&A 431, 111

15. The mass-energy output of NGC 7469 X-ray component 10.00239.6 X-ray component 20.0339.7 X-ray component 30.0239.4 UV component 10.00638.7 UV component 20.000438.7 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s -1 )

16. The mass-energy output of NGC 7469 X-ray component 10.00239.6 X-ray component 20.0339.7 X-ray component 30.0239.4 UV component 10.00638.7 UV component 20.000438.7 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s -1 ) The same gas

17. The mass-energy output of NGC 7469 X-ray component 10.00239.6 X-ray component 20.0339.7 X-ray component 30.0239.4 UV component 10.00638.7 UV component 20.000438.7 Total0.0640.1 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s -1 ) Using the X-ray phase properties for X1/UV2 The same gas

18. Conclusions We estimate that ~90% of the mass outflow rate and ~95% of the kinetic luminosity are associated with the soft X-ray absorbing components in this object. For a complete picture, we would also want to look at the highest-ionisation gas absorbing above 6 keV. Is this also the case for distant X-ray faint AGN (e.g. BALQSOs) for which we can only do optical spectroscopy? This has implications for attempts to infer the mass-energy output of cosmologically-interesting AGN winds from their rest-frame UV spectra. For further details see Blustin et al. 2007, A&A 466, 107