X-ray/UV Outflows and the

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Martin Ward, University of Durham
X-ray/UV Outflows and the Coronal Emission Lines
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Outflows are ubiquitous
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b
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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)
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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

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Coronal Line Diagnostics
Table from Oliva et al. (1994)
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Where are the Coronal Lines Emitted?
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Murayama and Taniguchi (1998)
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Where are the CLs emitted? Circinus Galaxy
Sey.2 (Oliva et al. 1994)
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Up-date on Circinus Sinfoni data Mueller
Sanchez et al (astro-ph Aug. 2005)
Narrow compact Broad spatially extended
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Chandra X-ray image of Circinus
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REJ1237264 IC3599, Brandt et al.1995
NLS1
1991.5
An extreme case with FeX, FeXI, FeXIV gt
OIII 5007
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IC3599 - Grupe et al (1995)see also Komossa and
Bade (1999)
1995.2
1992.1
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Kinematic information contained in the CL
profiles and shifts
Erkens et al. (1997)
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RE J1034396 KUG1031398
Puchnarewicz et al. (1995)
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KUG 1031398
See Casebeer et al. (2006), FUSE data plus
detailed photoionisation models
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Goncalaves et al (1999), KUG 1031398
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The Warm Absorber

• At least 50 of type 1 AGN have WAs
• 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?

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Cassidy and Raine (1997)
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PDS456 the radio quiet analogue of 3C273
evidence for outflows, X-ray/UV/IR CLs
Torres et al (1997)
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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

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X-ray Absorption in PDS 456
XMM-Newton RGS
XMM-Newton EPIC
No Iron K? Line
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Fe XVII XIX?
Fe XXV / XXVI ?
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Ultraviolet Properties of PDS 456
CIV ?1549 ?v shift -5000 km s-1
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?Ly? NV
Ly? BAL (14-20,000 km s-1) but no NV or CIV
absorption
HST Spectra of PDS 456 3C273, OBrien, Reeves
and Ward (2004)
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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
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Comparison of H? and Ly? profiles in PDS 456
H? black
Ly? red
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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
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Near IR Spec. of PDS456 comp. with 3C273
NGC4151
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Akn 564 Rodriquez-Ardila et al. (2002)
FeXIII I
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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?

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Concluding Remarks - specific

• CLs 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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