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QSO host galaxy properties from GEMS and COSMOS from z=0 to 3 Knud Jahnke

QSO host galaxy properties from GEMS and COSMOS from z=0 to 3 Knud Jahnke Max Planck Institute for Astronomy, Heidelberg. Sebasti á n F. S á nchez (CAHA) Lutz Wisotzki (AIP) +the GEMS team. Eva Schinnerer (MPIA) Vernesa Smolcic (MPIA) Chris Impey (U Arizona) Jared Gabor (U Arizona)

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QSO host galaxy properties from GEMS and COSMOS from z=0 to 3 Knud Jahnke

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  1. QSO host galaxy properties from GEMS and COSMOS from z=0 to 3 Knud Jahnke Max Planck Institute for Astronomy, Heidelberg Sebastián F. Sánchez (CAHA) Lutz Wisotzki (AIP) +the GEMS team Eva Schinnerer (MPIA) Vernesa Smolcic (MPIA) Chris Impey (U Arizona) Jared Gabor (U Arizona) +the COSMOS team(s)

  2. Goals: state & evolution of QSO host galaxies • role in general galaxy formation • GEMS: 80 broad line QSOs (55 @ z<3) • optically selected (COMBO17) • photo-z‘s (COMBO17) • ACS imaging F606W (=V), F850LP (=z) • COSMOS: 120 broad line QSOs (25 March 06) • optically selected (SDSS & SDSS+MMT) • radio selected (VLA-COSMOS) • spectro-z‘s (IMACS, zCOSMOS, SDSS) • ACS imaging F814W (=i)

  3. S COSMOS 120 QSOs Broad-line AGN sample: redshift distribution (z<3) 55 QSOs GEMS

  4. 2“ 500 stars 4500 stars 500 stars F606W (GEMS) F814W (COSMOS) F850LP (GEMS)

  5. >4% of residual flux „Resolved“ point sources: stars minus PSF 10% of objects Frequency Normalized subtraction residual

  6. z = 0.3–0.7 0.9–1.0 1.0–1.15 1.15–1.3 1.3–1.5 1.5–1.6 1.6–1.8 1.8–1.9 1.9–2.1 2.1–2.9 COSMOS ACS F814W 4“

  7. z=0.65 z=1.53 z=2.16 z=2.24

  8. >4% of residual flux Resolved QSOs: QSO minus PSF Frequency Normalized subtraction residual

  9. z = 0.3–0.7 0.9–1.0 1.0–1.15 1.15–1.3 1.3–1.5 1.5–1.6 1.6–1.8 1.8–1.9 1.9–2.1 2.1–2.9

  10. Current status & knowledge • COSMOS: ~50 resolved type 1 QSO hosts • GEMS: ~45 resolved (with optical colour) • Sanchez et al. 2004 • Jahnke et al. 2004 • Jahnke et al. (in prep) • Others: Kukula/Dunlop et al., Hutchings et al., Falomo et al., Kuhlbrodt et al. (at high z, 1–10 objects each)

  11. GEMS & ground based colours B&C03 (solar) disk dominated bulge dominated undecided

  12. GEMS z=0.7 Kormendy relation z=0.7 z=0

  13. COSMOS: host galaxy luminosities

  14. COSMOS+GEMS: homogeneous inactive comparison samples z=0.6 z=1.0

  15. Radio detected COSMOS+GEMS combined

  16. Results • BL QSO host galaxies span colour range from reddish to blue  contribution of young stars • Bulge-dominated and elliptical hosts can be substantially bluer than inactive counterparts • Confirmed for z=0 to 1.1 (SDSS+HES+GEMS) • Merger/distortion fraction seems increased (to be tested!) • Moderate to substantial SF at z~2, similar to LBGs • Radio selected QSO hosts @z=1 are more luminous than optically selected

  17. Diagnostic power • Differential host galaxy evolution compared to inactive galaxies • Influence of interaction on QSO activity (from merger fraction) • Test unified model for AGN from radio loud—quiet & type 1—type 2 comparison (luminosities, morphology) • QSO host galaxy parent population • With 2nd COSMOS HST band: spectrum of interaction strength triggering AGN activity (7/120 QSOs with NICMOS data)

  18. TBD • Full sample definition and selection description • Time variable PSF • 2d modelling + peak subtraction • Morphology analysis (Galfit et al.), direct comparison to inactive sample • Analysis of radio properties

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