Inflow… Outflow… Outflow… X-ray/UV Outflows and the Coronal Emission Lines Martin Ward, University of Durham
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 “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)
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
Coronal Line Diagnostics Table from Oliva et al. (1994)
Where are the Coronal Lines Emitted?
Murayama and Taniguchi (1998)
Where are the CL’s emitted? Circinus Galaxy – Sey.2 (Oliva et al. 1994)
Up-date on Circinus – Sinfoni data Mueller Sanchez et al (astro-ph Aug. 2005) Narrow = compact Broad = spatially extended
Chandra X-ray image of Circinus
REJ = IC3599, Brandt et al.1995 An extreme case with [FeX], [FeXI], [FeXIV] > [OIII] NLS1
IC Grupe et al (1995) see also Komossa and Bade (1999)
Erkens et al. (1997) Kinematic information contained in the CL profiles and shifts
RE J = KUG Puchnarewicz et al. (1995)
KUG See Casebeer et al. (2006), FUSE data plus detailed photoionisation models
Goncalaves et al (1999), KUG
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?
Cassidy and Raine (1997)
PDS456: the radio quiet analogue of 3C273 evidence for outflows, X-ray/UV/IR CL’s Torres et al (1997)
PDS456: The Most Luminous Nearby Quasar A luminosity normalised NLQSO L BOL = erg s -1, z= 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. ~ erg s -1 (10% L bol ) Highly variable in X-rays Properties consistent with high accretion-rate object
X-ray Absorption in PDS 456 No Iron K Line Fe XVII – XIX Fe XXV / XXVI XMM-Newton EPIC XMM-Newton RGS XMM-Newton RGS
HST Spectra of PDS 456 & 3C273, O’Brien, Reeves and Ward (2004) CIV 1549 v shift km s -1 Ly +NV Ly BAL (14-20,000 km s -1 ) – but no NV or CIV absorption Ultraviolet Properties of PDS 456
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
Comparison of H and Ly profiles in PDS 456 H black Ly red
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
Near IR Spec. of PDS456 + comp. with 3C273 & NGC4151
Akn 564 – Rodriquez-Ardila et al. (2002) [FeXIII] I
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?
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)