ACCRETIONACCRETION WINDSWINDS

Inflow…Inflow… Outflow…Outflow…

X-ray/UV Outflows and theCoronal 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 = compactBroad = spatially extended

Chandra X-ray image of Circinus

REJ1237+264 = IC3599, Brandt et al.1995

An extreme case with [FeX],[FeXI], [FeXIV] > [OIII] 5007

1991.5NLS1

IC3599 - Grupe et al (1995)see also Komossa and Bade (1999)

1995.2

1992.1

Erkens et al. (1997)

Kinematic information contained in the CL profiles and shifts

RE J1034+396 = KUG1031+398

Puchnarewicz et al. (1995)

KUG 1031+398

See Casebeer et al. (2006), FUSE data plus detailed photoionisation models

Goncalaves et al (1999), KUG 1031+398

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 • 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

X-ray Absorption in PDS 456

No Iron K Line

Fe XVII – XIX

Fe XXV / XXVI

XMM-Newton EPICXMM-Newton EPIC XMM-Newton RGSXMM-Newton RGS

HST Spectra of PDS 456 & 3C273, O’Brien, Reeves and Ward (2004)

CIV 1549 v shift -5000 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)