Date post: | 14-Dec-2015 |
Category: |
Documents |
Upload: | tyson-bisby |
View: | 214 times |
Download: | 0 times |
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