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The mass-energy budget of the ionised outflow in NGC 7469

The mass-energy budget of the ionised outflow in NGC 7469. Alexander J. Blustin. STFC Postdoctoral Fellow, UCL Mullard Space Science Laboratory.

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The mass-energy budget of the ionised outflow in NGC 7469

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  1. The mass-energy budget of the ionised outflow in NGC 7469 Alexander J. Blustin STFC Postdoctoral Fellow, UCL Mullard Space Science Laboratory 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) Chandra X-ray Gratings Meeting, Cambridge, MA, 11th July 2007

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

  3. Blustin et al. 2007, A&A 466, 107 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 (G = 1.81) plus soft excess (we used a 0.144 keV blackbody component). Significant soft X-ray residuals are visible

  4. The X-ray absorption and emission features Blustin et al. 2007, A&A 466, 107 Significance of narrow spectral features Dc2 = 16 implies 4s significance

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

  6. Absorption Measure Distribution (AMD) The AMD expresses the total line-of-sight column density as an integral over its distribution in log x NHtotal = (3.3 ± 0.8) x 1021 cm-2 Blustin et al. 2007, A&A 466, 107 Two main ionisation regimes: most gas at higher levels of ionisation See talk by Tomer Holczer for more details on AMDs

  7. Photoionised absorber modelling Blustin et al. 2007, A&A 466, 107 Scott et al. 2005 SED for Chandra/FUSE data Blustin et al. 2007 SED for XMM-Newton data 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

  8. Photoionised absorber modelling 3 absorber components: X-ray 1 X-ray 2 X-ray 3 Log x = 0.8+0.4-0.3 Log NH = 19.5 ± 0.2 cm-2 v = -2300 ± 200 km s-1 Log x = 2.73 ± 0.03 Log NH = 21.30+0.04-0.05 cm-2 v = -720 ± 50 km s-1 Log x = 3.56+0.08-0.07 Log NH = 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. UV properties from Scott et al. 2005 Comparison with UV-absorbing outflow Ionic columns (1014 cm-2) Log x v (km/s) NCIV NNV NHI UV 1 1.61 562 ± 6 0.98 ± 0.09 2.9 ± 0.8 7 ± 2 UV2 0.51 1901 ± 6 2.0 ± 0.1 2.5 ± 0.2 2.4 ±0.5 X-ray 1 0.8+0.4-0.3 2300 ± 200 1.6 3.4 6.2 X-ray 2 2.73 ± 0.03 720 ± 50 n/a 0.00091 n/a X-ray 3 3.56+0.08-0.07 580+80-50 n/a n/a n/a

  11. UV properties from Scott et al. 2005 Comparison with UV-absorbing outflow Ionic columns (1014 cm-2) Log x v (km/s) NCIV NNV NHI UV 1 1.61 562 ± 6 0.98 ± 0.09 2.9 ± 0.8 7 ± 2 UV2 0.51 1901 ± 6 2.0 ± 0.1 2.5 ± 0.2 2.4 ±0.5 X-ray 1 0.8+0.4-0.3 2300 ± 200 1.6 3.4 6.2 X-ray 2 2.73 ± 0.03 720 ± 50 n/a 0.00091 n/a X-ray 3 3.56+0.08-0.07 580+80-50 n/a n/a n/a Identify UV component 2 with X-ray component 1

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

  13. Momentum of outflowing matter Momentum of radiation absorbed and scattered by wind ~ Calculating the mass and energy transport of the outflow . 1.23 mproton Lion Cv v W Mass outflow rate, Mout ~ x Volume filling factor of the outflow obtained from the assumption that, for a radiatively driven wind: Blustin et al. 2005, A&A 431, 111

  14. . 1 Mout v2 2 Calculating the mass and energy transport of the outflow . 1.23 mproton Lion Cv v W Mass outflow rate, Mout ~ x (Labs + Lscatt) x Volume filling factor, Cv ~ 1.23 mproton c Lion v2W Kinetic luminosity, LKEout = Blustin et al. 2005, A&A 431, 111

  15. The mass-energy output of NGC 7469 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s-1) X-ray component 1 0.002 39.6 X-ray component 2 0.03 39.7 X-ray component 3 0.02 39.4 UV component 1 0.006 38.7 UV component 2 0.0004 38.7

  16. The mass-energy output of NGC 7469 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s-1) X-ray component 1 0.002 39.6 X-ray component 2 0.03 39.7 X-ray component 3 0.02 39.4 UV component 1 0.006 38.7 UV component 2 0.0004 38.7 The same gas

  17. The mass-energy output of NGC 7469 Mass outflow rate (Solar masses per year) Log Kinetic Luminosity (erg s-1) X-ray component 1 0.002 39.6 X-ray component 2 0.03 39.7 X-ray component 3 0.02 39.4 UV component 1 0.006 38.7 UV component 2 0.0004 38.7 Total 0.06 40.1 The same gas Using the X-ray phase properties for X1/UV2

  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

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