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Insights into AGN Host Galaxies: Observational Clues for AGN Feedback Mechanisms

Explore the intriguing properties of AGN host galaxies and their potential implications for AGN feedback mechanisms. Discover key observations related to optical luminosities, host masses, structure/morphology, stellar composition, ISM state, and kinematical structures across different redshifts. Uncover the characteristics of Type 1 QSO host galaxies and their unique features, such as luminosity, mass, composition, and kinematic distortions in the ISM. Gain insights into the link between AGN activity and the properties of their host galaxies.

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Insights into AGN Host Galaxies: Observational Clues for AGN Feedback Mechanisms

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  1. The properties of AGN host galaxies: Any clues for AGN feedback? Knud Jahnke, MPIA Collaborators: GEMS team (Chien, Hans-Walter, Klaus, Rachel + 15) Lutz Wisotzki, Malte Schramm, Bernd Husemann (AIP) Geraldine Letawe, Pierre Magain (Liege), Frederic Courbin (Lausanne) + 5 COSMOS team (Eva, Vernesa, Alejo, Frank, Martin +100)

  2. QSO host galaxies have… • …luminosities • …masses • …structure/morphology • …stellar composition • …ISM state • …kinematical structures • (some of this) can be observed from z=0 to 3

  3. Optical luminosities: low-z • z~0.1: luminous in the optical/NIR Jahnke & Wisotzki 2003; McLeod & Rieke 1994, 1995

  4. Optical luminosities: high-z • VLT NIR AO/nonAO imaging, z=2…3 • Host: luminous in rest-frame optical Schramm, Wisotzki, Jahnke 2007 Kuhlbrodt, Wisotzki, Örndahl, Jahnke 2005

  5. z = 0.3–0.7 0.9–1.0 1.0–1.15 1.15–1.3 1.3–1.5 1.5–1.6 1.6–1.8 1.8–1.9 1.9–2.1 2.1–2.9 COSMOS ACS F814W 4“

  6. z=0.65 z=1.53 z=2.16 z=2.24

  7. Optical luminosities: high-z • HST ACS imaging, GEMS+COSMOS (first year XMM+z sample) • Inactive galaxies: MK-limited sample from GOODS-MUSIC • Host galaxies: luminous in rest-frame UV to optical Jahnke, Sanchez et al. 2004b; Sanchez, Jahnke et al. 2004; Jahnke et al. in prep.

  8. Host masses: low-z • SDSS type 2 AGN • Massive galaxies • Correlated with Lnuc Kauffmann et al. 2003

  9. QSO host masses: high-z • VLT NIR color imaging • Host: massive @ z=2…3 • But high MBH compared to local Schramm, Wisotzki, Jahnke 2007

  10. Structure/morphology • E-CDFS/GEMS with HST/ACS • At z=0.7: Early type QSO hosts are on normal mag-size relation z=0 z=0.7 Sanchez, Jahnke et al. 2004

  11. Structure/morphology • ACS-COSMOS • No early-phase merger, but many asymmetries and non-relaxed systems • Unclear if merger fraction is enhanced compared to inactive COSMOS: Gabor, Jahnke, et al. in prep.

  12. Structure/morphology • But sometimes definitely violent… HE0450-2958 Magain et al. 2005, Nature

  13. Stellar composition: low-z • 20 type 1 QSOs, z~0.1 • Multiband imaging • Always young stars • Also for bulge dominated/early type hosts Late type Early type Jahnke et al. 2003, 2004

  14. Stellar composition: low-z • SDSS type 2 AGN • More young stars in strong AGN hosts Kauffmann et al. 2003

  15. Interlude: Type 1 QSO spectroscopy, on nucleus

  16. Type 1 QSO spectroscopy, on nucleus

  17. Type 1 QSO spectroscopy, on nucleus • 20 type 1 QSOs • 0.05<z<0.35 • Imaging available (VLT and some ACS) Jahnke et al. 2007; Letawe et al. 2007

  18. Stellar composition: low-z • Non-old, red and dead even for early types Letawe et al. 2007

  19. Stellar composition: high-z • Type 1 QSO host galaxies can have blue colours at any z Jahnke, Sanchez et al. 2004b; Sanchez, Jahnke et al. 2004; Jahnke et al. in prep.

  20. Stellar composition: high-z SSP models: B&C03 (solar) • Independent of dominant morphology Jahnke, Sanchez et al. 2004b; Sanchez, Jahnke et al. 2004; Jahnke et al. in prep. disk dominated bulge dominated undecided

  21. ISM state • PMAS Integral Field Spectroscopy • 20 QSOs, MV~23…25 • Extended Emission Line Regions • Out to several kpc radius Husemann, Wisotzki, Jahnke in prep.

  22. ISM state • No radio jet in EELR • Anticorrelation: FeII emission and kpc-extended [OIII] • 50% of EELR with desturbed velocity structure Husemann, Wisotzki, Jahnke in prep.

  23. ISM state • EELR [OIII] not correlated with nuclear continuum, but with nuclear [OIII] logL([OIII, EELR]) logL([OIII], AGN) logλLλ(5100A) Husemann, Wisotzki, Jahnke in prep.

  24. ISM state • VLT long-slit: ionisation by AGN out to many kpc Letawe et al. 2007; Jahnke et al. 2007

  25. Kinematical structures • Some perfect rotation curves • Some severely distorted velocity structures • Velocities several 100km/s • Merging? Inflow? Outflow? • PMAS IFS: 50% of EELRs with distorted velocity fields Letawe et al. 2007

  26. Take home summary: QSO hosts • Type 1 QSO host galaxies… • …are luminous and massive • …are bulge dominated but can have disk components • …are often asymmetric (tbd: relative to inactive?) • …lie near mag-size relation of inactive early types • …have often younger stellar pops compared to inactive early types (tbd: E+A or current SF?); particularly for distorted systems • …have large-scale AGN-ionized ISM, sometimes as ionisation cones • …have often large-scale kinematical distortions in ISM • …don‘t differ much between z=2 and z=0

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