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

Feedback between circumnuclear gas and AGN: implications for the AGN structure. Matteo Guainazzi, Stefano Bianchi a European Space Astronomy Center of ESA Villafranca del Castillo, Spain. Collaborators : M.Chiaberge (STScI), G.Matt, G.C.Perola (Roma Tre), E.Piconcelli (OAR).

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

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  1. 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, A&A, 444, 119 Bianchi et al., 2006a, A&A, 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

  2. (Ho et al. 1997) (Courtesy of Dr. Keel) 1021.5 cm-2 M82 ? 1025.5 cm-2 ? (Wilman & Fabian 1999) Outline (type 2 AGN should be soft X-ray silent ...) (Antonucci & Miller 1985)

  3. ASCA Actual soft X-ray luminosity Predicted starburst contribution 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)

  4. Soft X-ray extended emission and NLR Images: O[III] – Contours: soft X-rays 500 pc 600 pc 600 pc 600 pc Circinus Galaxy (Smith & Wilson 2001) NGC4151 (Yang et al. 2001) NGC5643 (Bianchi et al. 2006a) NGC1386 (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)

  5. Comparison with photoionization codes (CLOUDY) (Bianchi et al. 2006) Acceptable solutions in the density vs. ionization parameter plane Constant O[III] 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. theionization 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).

  6. OVIII/OVII excess is NOT coincident with star formation regions! … of course this is too simple NGC7582 Bianchi et al., 2007

  7. No continuum;  log(NH ) 22.7 Narrow RRC features:  photoionised plasma kT ~ 35,000-40,000 K He-like triplet diagnostic andhigher order series linesrule out a collisionally ionized plasma, and requires a contribution from photoexcitation NGC1068 senza segreti (Kinkhabwala et al. 2002) Starburst contribution to soft X-rays constrained to be 10%

  8. Circinus Chandra HETGS Sambruna et al. 2001 Sako et al. 2000 NGC4151 XMM RGS Schurch et al. 2004 The high resolution view

  9. 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)

  10. 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: LX≈1039 erg s-1 • young stellar cluster: LX≈6×1038 erg s-1 Levenson et al. 2005

  11. So… AGN or starburst? AGN -Total LO≥1040 erg s-1 -OVII/OVIII≥1 STARBURST Empirical diagnostic diagram based on high resolution spectroscopy Guainazzi & Bianchi, submitted

  12. Kaspi et al. (2000) Seyfert 1 Seyfert 2 Sako et al. (2000) •   1-1000 • NH  1021-22 cm-2 • Occam´s razor BH Torus (Kinkhabwala 2003)

  13. Summary • Highly X-ray emitting ionized gas on scales 102-103 pc • Morphology remarkably coincident with NLR • Observed O[III] 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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