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

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

0.3–0.70.3–0.7

0.9–1.00.9–1.0

1.0–1.151.0–1.15

1.15–1.31.15–1.3

1.3–1.51.3–1.5

1.5–1.61.5–1.6

1.6–1.81.6–1.8

1.8–1.91.8–1.9

1.9–2.11.9–2.1

2.1–2.92.1–2.9

z =z =C

OS

MO

S A

CS F

81

4W

CO

SM

OS A

CS F

81

4W

4“4“

z=2.24z=2.24z=2.16z=2.16

z=1.53z=1.53

z=0.65z=0.65

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.

Kauffmann et al. 2003

Host masses: low-z

SDSS type 2 AGN

Massive galaxies

Correlated with Lnuc

Schramm, Wisotzki, Jahnke 2007

QSO host masses: high-z VLT NIR color imaging

Host: massive @ z=2…3

But high MBH compared to local

z=0.7z=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

HE0450-2958

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

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

Stellar composition: low-z

Letawe et al. 2007

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 dominated bulge dominated undecided

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, MV~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

])

logλLλ(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