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Probing AGN Outflows with Variability

Probing AGN Outflows with Variability. Smita Mathur Ohio State. Collaborators: Yair Krongold, Fabrizio Nicastro, Anjali Gupta Nancy Brickhouse, Martin Elvis. Outburst in NGC 2617. Seyfert 1.8  Seyfert 1. Swift monitoring. + XMM. Outflows are ubiquitous.

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Probing AGN Outflows with Variability

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  1. Probing AGN Outflows with Variability Smita Mathur Ohio State Collaborators: Yair Krongold, Fabrizio Nicastro, Anjali Gupta Nancy Brickhouse, Martin Elvis

  2. Outburst in NGC 2617

  3. Seyfert 1.8  Seyfert 1

  4. Swift monitoring + XMM

  5. Outflows are ubiquitous Seen in 50% of Seyfert galaxies. NGC 3783 HST and FUSE

  6. Kaspi +

  7. Physical models of outflow • Accretion disk winds: Proga et al. - small physical scale • Winds off obscuring torus: Krolik & Kriss - on pc to 10s of pc scale • Outflowing NLR • Host galaxy ISM

  8. Disk winds Elvis 2000

  9. Proga +

  10. AGN outflows • Ubiquitous • Location, physical properties not well known until recently • Accretion disk winds? • Dependence on black hole mass/ Eddington luminosity ratio

  11. What is the distance of the absorber from the nucleus? Proposals span a factor of > 106 from accretion disk to Kpc scale narrow line region n R2

  12. How to measure the density? • Metastable absorption lines. - He I*, C II*, C III* - low ionization lines : distinct parameter space - Non-detection NOT constraining • Variability

  13. Variability Density Distance

  14. There can be variability due to absorber crossing line of sight. But Absorber must vary in responses to changes in ionizing continuum.

  15. Why is this a hard measurement? • X-rays: Integration times too large (one day = 86.4 ks) • UV: need many observations with dense time sampling  lots of HST orbits

  16. XMM Observations of NGC 4051 • RGS  High resolution spectrum • EPIC  Variability

  17. The Powerful UTA

  18. Log count rate Log U Log U 0 2 10 Time 104 s

  19. Krongold et al. 2007

  20. R (HIP) = 0.5-1.0 lt days. (2300-4600 RS) R (LIP) = < 3.5 lt days. (< 15800 RS) BH mass in NGC 4051 is 2 x 106 M⊙

  21. The outflow is clearly compact …consistent with an accretion disk origin. Rule out various models: - wind off torus edge (Krolik & Kriss) - continuous range of ionization parameter (Ogle et al.)

  22. Mass & Energy outflow rates HIP & LIP mass outflow rates: ~ 1 x 10-4 M⊙ yr-1 c.f. accretion rate: ~ 5 x 10-3 M⊙ yr-1

  23. Kinetic power released: ~1038 erg/s c.f. bolometric luminosity: 2.5 x 1043 erg/s Energy injection rate in the surrounding medium is significantly smaller than that required by feedback models Scannapieco Silk

  24. Observational evidence for accretion disk winds is scarce Short time-scale variability remains an unexplored region of the parameter space.

  25. Sparse sampling naturally leads to large radial distance. • Often radial distance is assumed to be that with escape velocity = outflow velocity. • Distance derived from metastable states is assumed for high ionization outflow.

  26. …..But what about luminous quasars? Dietrich et al. in prep.

  27. Seyferts are NOT scaled down Quasars L Merger Merger Z Secular Secular

  28. Future directions • Intra-day time resolved spectroscopy • X-ray: XMM advantage -- CCD and gratings • UV: HST COS -- exquisite sensitivity

  29. Discovery of relativistic outflows in soft X-rays

  30. Robust detection V ~ 0.1c Gupta et al. 2013

  31. Magneto-hydrodynamic wind? Gupta et al. 2013b

  32. Stay tuned….

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