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

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 Jahnke & Wisotzki 2003; McLeod & Rieke 1994, 1995   z~0.1: luminous in the optical/NIR

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. 0.3–0.70.9–1.01.0–1.151.15–1.31.3–1.51.5–1.61.6–1.81.8–1.91.9–2.12.1–2.9 z = COSMOS ACS F814W 4“

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

7. Optical luminosities: high-z  HST ACS imaging, GEMS+COSMOS (first year XMM+z sample)  Inactive galaxies: M K -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. Kauffmann et al. 2003 Host masses: low-z  SDSS type 2 AGN  Massive galaxies  Correlated with L nuc

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

10. z=0.7 z=0 Structure/morphology  E-CDFS/GEMS with HST/ACS  At z=0.7: Early type QSO hosts are on normal mag-size relation 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… Magain et al. 2005, Nature HE0450-2958

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

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.  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 Letawe et al. 2007   Non-old, red and dead even for early types

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. disk dominatedbulge dominatedundecided SSP models: B&C03 (solar) Stellar composition: high-z  Independent of dominant morphology Jahnke, Sanchez et al. 2004b; Sanchez, Jahnke et al. 2004; Jahnke et al. in prep.

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

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

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

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