Presentation on theme: "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,"— Presentation transcript:
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:
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
Optical luminosities: low-z Jahnke & Wisotzki 2003; McLeod & Rieke 1994, 1995 z~0.1: luminous in the optical/NIR
0.3–0.70.9–1.01.0– –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“
z=2.24 z=2.16 z=1.53 z=0.65
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.
Kauffmann et al Host masses: low-z SDSS type 2 AGN Massive galaxies Correlated with L nuc
Schramm, Wisotzki, Jahnke 2007 QSO host masses: high-z VLT NIR color imaging Host: z=2…3 But high M BH compared to local
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
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.
Structure/morphology But sometimes definitely violent… Magain et al. 2005, Nature HE
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
Stellar composition: low-z SDSS type 2 AGN More young stars in strong AGN hosts Kauffmann et al. 2003
Interlude: Type 1 QSO spectroscopy, on nucleus
Type 1 QSO spectroscopy, on nucleus
20 type 1 QSOs 0.05
Stellar composition: low-z Letawe et al Non-old, red and dead even for early types
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.
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.
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.
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
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]
ISM state VLT long-slit: ionisation by AGN out to many kpc Letawe et al. 2007; Jahnke et al. 2007
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
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