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ACCRETION

ACCRETION. WINDS. Inflow…. Outflow…. Martin Ward, University of Durham. X-ray/UV Outflows and the Coronal Emission Lines. Outflows are ubiquitous. b. Winds in general. Analogy with jets, they can tell us about bulk energy transport, and provide an imprint of past activity

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ACCRETION

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  1. ACCRETION WINDS Inflow… Outflow… Martin Ward, University of Durham X-ray/UV Outflows and the Coronal Emission Lines

  2. Outflows are ubiquitous

  3. b

  4. Winds in general • Analogy with jets, they can tell us about bulk energy transport, and provide an imprint of past activity • “May” give information on link between accretion disc and corona and high/low states of activity cf. galactic BH systems • Feedback - depends on mass outflow rate, and duty cycle For a good review on AGN winds see Crenshaw , Kraemer and George Ann. Revs. 194, 117 (2003)

  5. Coronal lines as an outflow diagnostic: what we know about CLs • Very high I.P. (by definition), up to ~0.4 keV (thermal = 3 million K) • Sometimes (not always) very broad cf. the extended NLR profiles • Sometimes (not always) blue shifted peak w.r.t the NLR profiles • Sometimes they have obvious blue winged profile (multi-spatial components) • Variability? Not well understood but yes in a few cases, needs more studies

  6. Coronal Line Diagnostics Table from Oliva et al. (1994)

  7. Where are the Coronal Lines Emitted?

  8. Murayama and Taniguchi (1998)

  9. Where are the CL’s emitted? Circinus Galaxy – Sey.2 (Oliva et al. 1994)

  10. Up-date on Circinus – Sinfoni data Mueller Sanchez et al (astro-ph Aug. 2005) Narrow = compact Broad = spatially extended

  11. Chandra X-ray image of Circinus

  12. REJ1237+264 = IC3599, Brandt et al.1995 NLS1 1991.5 An extreme case with [FeX], [FeXI], [FeXIV] > [OIII] 5007

  13. IC3599 - Grupe et al (1995)see also Komossa and Bade (1999) 1995.2 1992.1

  14. Kinematic information contained in the CL profiles and shifts Erkens et al. (1997)

  15. RE J1034+396 = KUG1031+398 Puchnarewicz et al. (1995)

  16. KUG 1031+398 See Casebeer et al. (2006), FUSE data plus detailed photoionisation models

  17. Goncalaves et al (1999), KUG 1031+398

  18. The Warm Absorber • At least 50% of type 1 AGN have WA’s • X-ray absorption by ionised gas along our line of sight • Deep OVII and OVIII edges • Sensitive diagnostic of the ionisation structure and kinematics of the gas • Are the UV and X-ray absorbers related? Possibly diff. phases of gas at same velocity • Where are the absorbers located?

  19. Cassidy and Raine (1997)

  20. PDS456: the radio quiet analogue of 3C273 evidence for outflows, X-ray/UV/IR CL’s Torres et al (1997)

  21. PDS456: The Most Luminous Nearby Quasar A luminosity normalised NLQSO • LBOL = 1047 erg s-1 , z= 0.184 • PDS 456 is radio-quiet,so no jet contamination (cf. 3C 273) SUMMARY OF X-RAY DATA • Outflowing at ~ 0.15c • If hard X-rays driving outflow, mass-loss rate ~ 10 M yr-1 • If 10% covering factor, outflow K.E. ~ 1046 erg s-1 (10% Lbol) • Highly variable in X-rays • Properties consistent with high accretion-rate object

  22. X-ray Absorption in PDS456 XMM-Newton RGS XMM-Newton EPIC No Iron K Line  Fe XVII – XIX Fe XXV / XXVI

  23. Ultraviolet Properties of PDS 456 CIV 1549 v shift -5000 km s-1  Ly +NV Ly BAL (14-20,000 km s-1) – but no NV or CIV absorption HST Spectra of PDS 456 & 3C273, O’Brien, Reeves and Ward (2004)

  24. CIV velocity shifts in Sloan quasars (Richards et al. 2002) Dashed ones are recomputed by hand Blue shift for CIV in PDS456 is 4,000-5,000 km/s

  25. Comparison of H and Ly profiles in PDS 456 H black Ly red

  26. HST Ultraviolet Spectra of PDS 456 & NGC 3783 Showing narrow gal. absorption & broad intrinsic absorption which, if associated with Ly, has vel. shift 14,000 – 20,000 km/s

  27. Near IR Spec. of PDS456 + comp. with 3C273 & NGC4151

  28. Akn 564 – Rodriquez-Ardila et al. (2002) [FeXIII] I

  29. Concluding Remarks - general • Winds are important – 50 years of trying to understand accretion and relativistic jets, now turn of winds • What drives them of all scales – how are low and high velocity winds related? • What switches them on and off? • Can they tell us something fundamental about AGN physics and evolution?

  30. Concluding Remarks - specific • CL’s may be spatially coincident with the WA and/or the X-ray soft excess components. • If so they can be used as an additional or proxy measurement of its properties • They certainly contain information about kinematics inside the NLR and the SED in the UV/soft X-ray region • Now is a good time to revitalise the study of CLs – (near IR hi-res. spectra, IFUs and monitoring with robotic telescopes)

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