QSO host galaxy properties QSO host galaxy properties from GEMS and COSMOS from GEMS and COSMOS

from z=0 to 3from z=0 to 3Knud JahnkeKnud Jahnke

Max Planck Institute for Astronomy, HeidelbergMax Planck Institute for Astronomy, Heidelberg

SebastiSebastiáán F. Sn F. Sáánchez (CAHA)nchez (CAHA)

Lutz Wisotzki (AIP)Lutz Wisotzki (AIP)

+the GEMS team+the GEMS teamEva Schinnerer (MPIA)Eva Schinnerer (MPIA)

Vernesa Smolcic (MPIA)Vernesa Smolcic (MPIA)

Chris Impey (U Arizona)Chris Impey (U Arizona)

Jared Gabor (U Arizona)Jared Gabor (U Arizona)

+the COSMOS team(s)+the COSMOS team(s)

Goals: state & evolution of QSO host galaxies Goals: state & evolution of QSO host galaxies •role in general galaxy formation role in general galaxy formation

GEMS: 80 broad line QSOs (55 @ z<3)GEMS: 80 broad line QSOs (55 @ z<3)•optically selected (COMBO17)optically selected (COMBO17)•photo-z‘s (COMBO17)photo-z‘s (COMBO17)•ACS imaging F606W (=V), F850LP (=z)ACS imaging F606W (=V), F850LP (=z)

COSMOS: 120 broad line QSOs (25 March 06)COSMOS: 120 broad line QSOs (25 March 06)•optically selected (SDSS & SDSS+MMT)optically selected (SDSS & SDSS+MMT)•radio selected (VLA-COSMOS)radio selected (VLA-COSMOS)•spectro-z‘s (IMACS, zCOSMOS, SDSS)spectro-z‘s (IMACS, zCOSMOS, SDSS)•ACS imaging F814W (=i)ACS imaging F814W (=i)

SS

Broad-line AGN sample: Broad-line AGN sample: redshift distribution redshift distribution (z<3)(z<3)

55 QSOs55 QSOs

COSMOS

120 QSOs120 QSOs

GEMSGEMS

2“F606W(GEMS)

F850LP(GEMS)

F814W(COSMOS

)

500 stars

4500 stars

500 stars

10% of objects

„„Resolved“ point sources: stars minus Resolved“ point sources: stars minus PSFPSF

Normalized subtraction residual

Frequ

en

cy

>4% of residual flux

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

Resolved QSOs: QSO minus PSFResolved QSOs: QSO minus PSF

Freq

uen

cy

Normalized subtraction residual

>4% of residual flux

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 =

COSMOS: ~50 resolved type 1 QSO hostsCOSMOS: ~50 resolved type 1 QSO hosts

GEMS: ~45 resolved (with optical colour)GEMS: ~45 resolved (with optical colour)

•Sanchez et al. 2004Sanchez et al. 2004

•Jahnke et al. 2004Jahnke et al. 2004

•Jahnke et al. (in prep)Jahnke et al. (in prep)

Others: Kukula/Dunlop et al., Hutchings et al., Others: Kukula/Dunlop et al., Hutchings et al., Falomo et al., Kuhlbrodt et al. (at high z, 1–10 Falomo et al., Kuhlbrodt et al. (at high z, 1–10 objects each) objects each)

Current status & knowledgeCurrent status & knowledge

disk dominateddisk dominated bulge dominatedbulge dominated undecidedundecided

GEMS & ground based GEMS & ground based colourscolours

B&C03 B&C03 (solar)(solar)

GEMS z=0.7 Kormendy GEMS z=0.7 Kormendy relationrelation

z=0z=0z=0.7z=0.7

COSMOS: host galaxy luminositiesCOSMOS: host galaxy luminosities

z=0.6z=0.6 z=1.0z=1.0

COSMOS+GEMS: homogeneous COSMOS+GEMS: homogeneous inactive comparison samplesinactive comparison samples

COSMOS+GEMS combined COSMOS+GEMS combined

Radio detectedRadio detected

Results Results

•BL QSO host galaxies span colour range from BL QSO host galaxies span colour range from reddish to blue reddish to blue contribution of young stars contribution of young stars

•Bulge-dominated and elliptical hosts can be Bulge-dominated and elliptical hosts can be substantially bluer than inactive counterpartssubstantially bluer than inactive counterparts

•Confirmed for z=0 to 1.1 (SDSS+HES+GEMS)Confirmed for z=0 to 1.1 (SDSS+HES+GEMS)

•Merger/distortion fraction seems increased (to be Merger/distortion fraction seems increased (to be tested!)tested!)

•Moderate to substantial SF at z~2, similar to LBGsModerate to substantial SF at z~2, similar to LBGs

•Radio selected QSO hosts @z=1 are more Radio selected QSO hosts @z=1 are more luminous than optically selectedluminous than optically selected

Diagnostic power Diagnostic power

•Differential host galaxy evolution compared to Differential host galaxy evolution compared to inactive galaxiesinactive galaxies

•Influence of interaction on QSO activity (from Influence of interaction on QSO activity (from merger fraction)merger fraction)

•Test unified model for AGN from radio loud—quiet & Test unified model for AGN from radio loud—quiet & type 1—type 2 comparison (luminosities, morphology)type 1—type 2 comparison (luminosities, morphology)

•QSO host galaxy parent populationQSO host galaxy parent population

•With 2nd COSMOS HST band: spectrum of With 2nd COSMOS HST band: spectrum of interaction strength triggering AGN activity (7/120 interaction strength triggering AGN activity (7/120 QSOs with NICMOS data)QSOs with NICMOS data)

TBD TBD

•Full sample definition and selection descriptionFull sample definition and selection description

•Time variable PSFTime variable PSF

•2d modelling + peak subtraction2d modelling + peak subtraction

•Morphology analysis (Galfit et al.), direct Morphology analysis (Galfit et al.), direct comparison to inactive samplecomparison to inactive sample

•Analysis of radio propertiesAnalysis of radio properties