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AGN hosts at 0.05<z<2.7: Young stars and mergers?
Knud Jahnke (AIP), Lutz Wisotzki (AIP)
Sebastián F. Sánchez (AIP, CAHA/IAA)Björn Kuhlbrodt (AIP)
+ the GEMS collaboration:
Marco Barden, Eric Bell, Andrea Borch, Boris Häußler, Klaus Meisenheimer, Hans-Walter Rix (MPIA)
Steve Beckwith, Chien Peng, Rachel Somerville (STScI)
John Caldwell, Sharda Jogee (UT Austin)
Dan McIntosh (U Massachusetts)
Chris Wolf (Oxford)
© 2004, Knud Jahnke, http://www.aip.de/~jahnke
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AGN hosts at 0.05<z<2.7: Young stars and mergers?
Motivation:● Merger-AGN connection● Starburst-AGN connection
study type 1 AGN/quasar host galaxies up to high z● luminous AGN● large physical scales● colours/morphologies/asymmetries● use well selected samples
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AGN hosts at 0.05<z<2.7: Young stars and mergers?
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4 MB ~ -23
MB ~ -21.5
MB ~ -24.5
AGN samples
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Hamburg/ESO quasar survey: southern extragalactic sky
● optical objective prism survey● targets bright QSOs, 13<BJ<17.5
● flux limited sample of 415 bright QSOs
COMBO-17 (PI C. Wolf): 4 x 30' x 30', ● 17 bands (UBVRI + 12 medium)● object classification, incl. broad-line AGN● spectrophotometric redshifts● 8,000 stars● 150,000 galaxies● 35,000 redshifts (R<24)● ~300 BL AGN
AGN samples
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AGN samplesz<0.2: BVRIJHK ground based photometry
z>0.5: GEMS (PI H.-W. Rix) ● E-CDFS, 30' x 30'● 80 HST ACS pointings● F606W (=V) + F850LP (=z) bands, 1 orbit/pointing/band● ~80 BL AGN + ~500 X-ray AGN (Chandra)
3 sub-samples:● 0.5<z<1.1: V<4000Å, z>4000Å, optical-UV colour● 1.1<z<1.8: V<4000Å, UV luminosity only● 1.8<z<2.75: V+z<4000Å, UV-UV colour
for 1.5<z<2.0: NICMOS imaging, cycle 13 (31 orbits granted)● optical-UV colour
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AGN samples
Selection criteria:● z<0.2: HES, complete, optically flux limited● z>0.5: COMBO-17 AGN class● R<24 (MB=-20...-24)
● 'Host galaxy resolved' criterion: >5% of total flux● 0.5<z<1.8: 2d modelling with GALFIT (C. Y. Peng et
al.)
0.05<z<0.2: 19 total 19 resolved
0.5<z<1.1: 15 total 15 resolved
1.1<z<1.8: 19 total 13 resolved
1.8<z<2.75: 23 total 9 resolved
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AGN samples
Selection criteria:● z<0.2: HES, complete, optically flux limited● z>0.5: COMBO-17 AGN class● R<24 (MB=-20...-24)
● 'Host galaxy resolved' criterion: >5% of total flux● 0.5<z<1.8: 2d modelling with GALFIT (C. Y. Peng et
al.)
0.05<z<0.2: 19 total 19 resolved
0.5<z<1.1: 15 total 15 resolved
1.1<z<1.8: 19 total 13 resolved
1.8<z<2.75: 23 total 9 resolvedJahnke , Kuhlbrodt, Wisotzki, 2004, MNRAS, 325, 52
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0.05<z<0.2
HE 1254-0934, z=0.139
20 kpc
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0.05<z<0.2
HE 1300-1325, z=0.047
5 kpc
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0.05<z<0.2
HE 1029-1401, z=0.085
10 kpc
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Resolved: 19/19
Morphologies:
9/19: early type galaxies
10/19: late type galaxies
Distortions:
6/19: ongoing interaction
3/19: other asymmetries
0.05<z<0.2
~30-45% were/are tidally interacting
~55% show no signs of interaction
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0.05<z<0.2
optical-NIR colour-magnitude diagram
early type hosts
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Colours:
early type hosts blue compared to inactive (V-K)
as blue as late type hosts
but not starburst
young stellar component throughout host (not circumnuclear)
mix of young and underlying old
0.05<z<0.2
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AGN samples
Selection criteria:● z<0.2: HES, complete, optically flux limited● z>0.5: COMBO-17 AGN class● R<24 (MB=-20...-24)
● 'Host galaxy resolved' criterion: >5% of total flux● 0.5<z<1.8: 2d modelling with GALFIT (C. Y. Peng et
al.)
0.05<z<0.2: 19 total 19 resolved
0.5<z<1.1: 15 total 15 resolved
1.1<z<1.8: 19 total 13 resolved
1.8<z<2.75: 23 total 9 resolvedSánchez, Jahnke, Wisotzki, et al., 2004, ApJ, 614, 586
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0.5<z<1.1
COMBO-17 CDFS 42601, z=0.733
10 kpc
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0.5<z<1.1
COMBO-17 CDFS 15731, z=0.835
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0.5<z<1.1
COMBO-17 CDFS 47615, z=0.649
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0.5<z<1.1
COMBO-17 CDFS 39432, z=0.738
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Resolved: 15/15
Morphologies:
12/15: early type (by Sérsic fit)
3/15: likely disk dominated
Distortions:
4/15: probable ongoing interaction
3/15: other possible asymmetries
0.5<z<1.1
~25-50% were/are tidally interacting
~50% show no signs of interaction
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0.5<z<1.1
observed colours
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0.5<z<1.1
rest-frame colours
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0.5<z<1.1
Kormendy relation
z=0.7
z=0
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Colours of early type hosts:
5/12: globally blue
+4/12: at blue edge of red sequence
only 3/12: red
Host luminosities: MV=-18.5...-22.0
Stellar masses:
early type hosts right on z=0.7 Kormendy relation
so not unusual M/L, underlying old population?
0.5<z<1.1
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AGN samples
Selection criteria:● z<0.2: HES, complete, optically flux limited● z>0.5: COMBO-17 AGN class● R<24 (MB=-20...-24)
● 'Host galaxy resolved' criterion: >5% of total flux● 0.5<z<1.8: 2d modelling with GALFIT (C. Y. Peng et
al.)
0.05<z<0.2: 19 total 19 resolved
0.5<z<1.1: 15 total 15 resolved
1.1<z<1.8: 19 total 13 resolved
1.8<z<2.75: 23 total 9 resolved
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1.1<z<1.8
COMBO-17 CDFS 18256, z=1.647
10 kpc
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1.1<z<1.8
COMBO-17 CDFS 54839, z=1.428
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1.1<z<1.8
COMBO-17 CDFS 16155, z=1.285
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1.1<z<1.8
COMBO-17 CDFS 04050, z=1.635
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Resolved: 13/19
Morphologies:
2/13: likely disk dominated (by Sérsic fit)
11/13: undecidable
Distortions:
5/13 resolved, symmetric
1/5: knots (but likely PSF-structure)
2/5: nearby (<1.5'') companions
8/13 resolved with asymmetries or extensions
1.1<z<1.8
~60% were/are tidally interacting
~40% show no signs of interaction
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1.1<z<1.8
200nm luminosity/SFR vs. redshift
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Colours: N/A
Luminosities:
few 1028 erg/s/Å (at 200nm)
few Msun/yr star formation (if starforming)
not strong starburst
1.1<z<1.8
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AGN samples
Selection criteria:● z<0.2: HES, complete, optically flux limited● z>0.5: COMBO-17 AGN class● R<24 (MB=-20...-24)
● 'Host galaxy resolved' criterion: >5% of total flux● 0.5<z<1.8: 2d modelling with GALFIT (C. Y. Peng et
al.)
0.05<z<0.2: 19 total 19 resolved
0.5<z<1.1: 15 total 15 resolved
1.1<z<1.8: 19 total 13 resolved
1.8<z<2.75: 23 total 9 resolvedJahnke, Sánchez, Wisotzki, et al., 2004, ApJ, 614, 568
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1.8<z<2.75
COMBO-17 CDFS 05498, z=2.075
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1.8<z<2.75
COMBO-17 CDFS 11922, z=2.539
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1.8<z<2.75
UV spectral slope vs. 200nm mag
LBGs (z=2.5)
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1.8<z<2.75
200nm luminosity/SFR vs. redshift
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1.8<z<2.75
UV colour vs. redshift
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Colours: ● slightly UV-redder than LBGs● young stellar component● but not in starburst-phase
UV luminosities:● similar to LBGs● either: post-starburst young population● or: ongoing starformation (5 Msun/yr from UV)
1.8<z<2.75
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Some conclusions
many hosts:● globally young stellar populations, from z=0.1 to 2.8● many blue early type host galaxies● at z=2: UV light similar LBG
merging vs. no interaction (z<1.8):
z<0.2: 30% merger, 15% possibly interacting, 55% smooth
0.5<z<1.1: 25% merger, 25% possibly interacting, 50% smooth
1.1<z<1.8: 60% possibly interacting, 40% smooth
tentative: merger fraction increasing with z
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Some more conclusions
Two options: delay or gas rich E's
1) Delay/evolutionary sequence?● progenitor → merger/starburst → delay → AGN● colour: upper limit for delay (few 100 Myr)● (smooth) morphology: lower limit for delay (few 100 Myr)
2) Gas rich early type host plus intermittent AGN phase● explains smooth early type hosts● so is only gas-richness special?
Diagnostics?● stellar population age dating AGN hosts ● search for merger signs in smooth hosts
insert your favoritephysics here
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~fin~