1 Ringberg Castle Workshop on AGN Physics, 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,

2 Ringberg Castle Workshop on AGN Physics, 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

3 Ringberg Castle Workshop on AGN Physics, AGN hosts at 0.05<z<2.7: Young stars and mergers?

4 Ringberg Castle Workshop on AGN Physics, M B ~ -23 M B ~ M B ~ AGN samples

5 Ringberg Castle Workshop on AGN Physics, Hamburg/ESO quasar survey: southern extragalactic sky ● optical objective prism survey ● targets bright QSOs, 13<B J <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

6 Ringberg Castle Workshop on AGN Physics, AGN samples z<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: ● Å, 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

7 Ringberg Castle Workshop on AGN Physics, AGN samples Selection criteria: ● z<0.2: HES, complete, optically flux limited ● z>0.5: COMBO-17 AGN class ● R<24 (M B = ) ● '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 total19 resolved 0.5<z<1.1: 15 total15 resolved 1.1<z<1.8: 19 total13 resolved 1.8<z<2.75: 23 total9 resolved

8 Ringberg Castle Workshop on AGN Physics, AGN samples Selection criteria: ● z<0.2: HES, complete, optically flux limited ● z>0.5: COMBO-17 AGN class ● R<24 (M B = ) ● '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 total19 resolved 0.5<z<1.1: 15 total15 resolved 1.1<z<1.8: 19 total13 resolved 1.8<z<2.75: 23 total9 resolved Jahnke, Kuhlbrodt, Wisotzki, 2004, MNRAS, 325, 52

9 Ringberg Castle Workshop on AGN Physics, <z<0.2 HE , z= kpc

10 Ringberg Castle Workshop on AGN Physics, <z<0.2 HE , z= kpc

11 Ringberg Castle Workshop on AGN Physics, <z<0.2 HE , z= kpc

12 Ringberg Castle Workshop on AGN Physics, 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

13 Ringberg Castle Workshop on AGN Physics, <z<0.2 optical-NIR colour-magnitude diagram early type hosts

14 Ringberg Castle Workshop on AGN Physics, 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

15 Ringberg Castle Workshop on AGN Physics, AGN samples Selection criteria: ● z<0.2: HES, complete, optically flux limited ● z>0.5: COMBO-17 AGN class ● R<24 (M B = ) ● '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 total19 resolved 0.5<z<1.1: 15 total15 resolved 1.1<z<1.8: 19 total13 resolved 1.8<z<2.75: 23 total9 resolved Sánchez, Jahnke, Wisotzki, et al., 2004, ApJ, 614, 586

16 Ringberg Castle Workshop on AGN Physics, <z<1.1 COMBO-17 CDFS 42601, z= kpc

17 Ringberg Castle Workshop on AGN Physics, <z<1.1 COMBO-17 CDFS 15731, z=0.835

18 Ringberg Castle Workshop on AGN Physics, <z<1.1 COMBO-17 CDFS 47615, z=0.649

19 Ringberg Castle Workshop on AGN Physics, <z<1.1 COMBO-17 CDFS 39432, z=0.738

20 Ringberg Castle Workshop on AGN Physics, 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

21 Ringberg Castle Workshop on AGN Physics, <z<1.1 observed colours

22 Ringberg Castle Workshop on AGN Physics, <z<1.1 rest-frame colours

23 Ringberg Castle Workshop on AGN Physics, <z<1.1 Kormendy relation z=0.7 z=0

24 Ringberg Castle Workshop on AGN Physics, Colours of early type hosts: 5/12: globally blue +4/12: at blue edge of red sequence only 3/12: red Host luminosities: M V = 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

25 Ringberg Castle Workshop on AGN Physics, AGN samples Selection criteria: ● z<0.2: HES, complete, optically flux limited ● z>0.5: COMBO-17 AGN class ● R<24 (M B = ) ● '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 total19 resolved 0.5<z<1.1: 15 total15 resolved 1.1<z<1.8: 19 total13 resolved 1.8<z<2.75: 23 total9 resolved

26 Ringberg Castle Workshop on AGN Physics, <z<1.8 COMBO-17 CDFS 18256, z= kpc

27 Ringberg Castle Workshop on AGN Physics, <z<1.8 COMBO-17 CDFS 54839, z=1.428

28 Ringberg Castle Workshop on AGN Physics, <z<1.8 COMBO-17 CDFS 16155, z=1.285

29 Ringberg Castle Workshop on AGN Physics, <z<1.8 COMBO-17 CDFS 04050, z=1.635

30 Ringberg Castle Workshop on AGN Physics, 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

31 Ringberg Castle Workshop on AGN Physics, <z< nm luminosity/SFR vs. redshift

32 Ringberg Castle Workshop on AGN Physics, Colours: N/A Luminosities: few erg/s/Å (at 200nm) few M sun /yr star formation (if starforming) not strong starburst 1.1<z<1.8

33 Ringberg Castle Workshop on AGN Physics, AGN samples Selection criteria: ● z<0.2: HES, complete, optically flux limited ● z>0.5: COMBO-17 AGN class ● R<24 (M B = ) ● '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 total19 resolved 0.5<z<1.1: 15 total15 resolved 1.1<z<1.8: 19 total13 resolved 1.8<z<2.75: 23 total9 resolved Jahnke, Sánchez, Wisotzki, et al., 2004, ApJ, 614, 568

34 Ringberg Castle Workshop on AGN Physics, <z<2.75 COMBO-17 CDFS 05498, z=2.075

35 Ringberg Castle Workshop on AGN Physics, <z<2.75 COMBO-17 CDFS 11922, z=2.539

36 Ringberg Castle Workshop on AGN Physics, <z<2.75 UV spectral slope vs. 200nm mag LBGs (z=2.5)

37 Ringberg Castle Workshop on AGN Physics, <z< nm luminosity/SFR vs. redshift

38 Ringberg Castle Workshop on AGN Physics, <z<2.75 UV colour vs. redshift

39 Ringberg Castle Workshop on AGN Physics, 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 M sun /yr from UV) 1.8<z<2.75

40 Ringberg Castle Workshop on AGN Physics, 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

41 Ringberg Castle Workshop on AGN Physics, 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 favorite physics here

42 Ringberg Castle Workshop on AGN Physics, ~fin~