Feedback between circumnuclear gas and AGN: implications for the AGN structure

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Feedback between circumnuclear gas and AGN
implications for the AGN structure

• Matteo Guainazzi, Stefano Bianchia
• European Space Astronomy Center of ESA
• Villafranca del Castillo, Spain

Collaborators M.Chiaberge (STScI), G.Matt,
G.C.Perola (Roma Tre), E.Piconcelli (OAR)
Guainazzi et al., 2005, AA, 444, 119 Bianchi et
al., 2006a, AA, 448, 499 Bianchi et al., 2006b,
MNRAS, astro-ph/0610277 Guainazzi Bianchi,
MNRAS, submitted
anow at the Department of Physics E.Amaldi of
the Roma Tre University
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Outline (type 2 AGN should be soft X-ray silent
...)
(Antonucci Miller 1985)
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Soft X-ray excess in obscured AGN
Ubiquitous soft excess. Too steep to be due to
nuclear continuum scattering
Soft X-ray luminosity too large to be due to gas
mechanical heating
(Guainazzi et al. 2005)
(Turner et al. 1997)
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Soft X-ray extended emission and NLR
Images OIII Contours soft X-rays
500 pc
600 pc
600 pc
600 pc
Circinus Galaxy (Smith Wilson 2001)
NGC4151 (Yang et al. 2001)
NGC1386 (Bianchi et al. 2006a)
NGC5643 (Bianchi et al. 2006a)
500 pc
1000 pc
700 pc
2000 pc
NGC1068 (Young et al. 2001)
NGC5347 (Bianchi et al. 2006a)
Mkn3 (Sako et al. 2000)
NGC3393 (Bianchi et al. 2006a)
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Comparison with photoionization codes (CLOUDY)
(Bianchi et al. 2006)
Acceptable solutions in the density vs.
ionization parameter plane
Constant OIII to X-ray flux ratio requires ???
The comparison between the Chandra and the HST
images shows that the OIII/soft X-ray ratio is
fairly constant along with the radius, up to
hundreds of pc. Photoionization models reproduce
this behavior if ne?r-?, with ??2 (i.e. the
ionization parameter is ? constant). This is in
agreement with NLR emission line ratios (e.g.
Kraemer et al. 2000, Kraemer Crenshaw 2000,
Bradley et al. 2004, Collins et al. 2005).
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of course this is too simple
NGC7582
Bianchi et al., 2007
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NGC1068 senza segreti
(Kinkhabwala et al. 2002)
Starburst contribution to soft X-rays constrained
to be ?10
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The high resolution view
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RGS sample results (66 Seyfert 2s)
(Guainazzi Bianchi, submitted)
Large fraction (?40) of narrow Radiative
Recombination Continua Higher order resonance
transitions (np?1s) larger then in pure
photoionization ? AGN-photoionization (with
important role of resonant scattering)
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What about the starburst contribution?
Jiménez-Bailón et al. 2003
NGC7130
NGC4303
HST
Chandra
3 pc
110 pc

• In the immermost 110 pc
• low luminosity AGN LX1039 erg s-1
• young stellar cluster LX61038 erg s-1

Levenson et al. 2005
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So AGN or starburst?
Empirical diagnostic diagram based on high
resolution spectroscopy
Guainazzi Bianchi, submitted
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Kaspi et al. (2000)
Seyfert 1
Seyfert 2
Sako et al. (2000)

• ? ? 1-1000
• NH ? 1021-22 cm-2
• Occams razor

BH
Torus
(Kinkhabwala 2003)
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Summary

• Highly X-ray emitting ionized gas on scales
  102-103 pc
• Morphology remarkably coincident with NLR
• Observed OIII to X-ray fluxes consistent with
  ne? r-2
• Origin AGN photoionization ...
• ... with important contribution by resonant
  scattering
• Star formation processes do not dominate the
  energy budget in soft X-rays
• A fraction of Seyfert/Starburst composite
  objects unveils in X-rays
• Purely X-ray diagnostic to discriminate on a
  statistical basis between starburst- and
  AGN-powered sources
• Warm scattering vs. warm absorber
• Measured observables consistent with being the
  same gas seen at different angles

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Seyferts vs. starbursts
(Guainazzi Bianchi, submitted)
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Proprietà generali degli assorbitori ionizzati
Parametro di ionizzazione
Densità
(Blustin et al. 2005)
Densità e parametro di ionizzazione degli
assorbitori ionizzati (warm absorbers) in
oggetti di tipo 1 coprono lo stesso intervallo di
parametri del warm scattering in oggetti di tipo 2