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mpia.de/coevolution

Dynamical masses of lensed quasar host galaxies at z~2: Near Infrared Integral Field Spectroscopy with Laser Adaptive Optics Knud Jahnke 1 , Katherine J. Inskip 1 , Hans-Walter Rix 1 , Chien Y. Peng 2 1 MPI Astronomy, 2 Herzberg Inst. of Astrophysics. www.mpia.de/coevolution. M BH /M sun.

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mpia.de/coevolution

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  1. Dynamical masses of lensed quasar host galaxies at z~2: Near Infrared Integral Field Spectroscopy with Laser Adaptive Optics Knud Jahnke1, Katherine J. Inskip1, Hans-Walter Rix1, Chien Y. Peng2 1MPI Astronomy, 2Herzberg Inst. of Astrophysics • www.mpia.de/coevolution

  2. MBH/Msun M* /Msun z=0: Häring&Rix 2004 Science goal Co-evolution of Black Holes and galactic bulges: • Tight correlation of MBH and Mbulge (0.3dex scatter) • Linear scales differ by ~1,000,000,000 • Which is physical mechanism? AGN Feedback? • Sims: not from first principles • Goal: Empirically constrain evolution of relation  Friday morning plenary talks

  3. ~1.5“ Target(s): Gravitationally lensed quasars Need quasars: • MBH from broad emission lines • access to host galaxy difficult Lens: boost in • Flux • Angular scale • Host galaxy „easier“ analysis HE0047–1756, z=1.67 Double AGN, Einstein ring HST NICMOS (H-band) original AGN subtracted  Try dynamical masses: H @1.75mu

  4. IFS with Laser Guide Star Adaptive Optics No AO: Atmosphere resolution limit Natural guidestar AO: AO correction, ~few % sky coverage Laser guidestar AO: AO correction, ~50% sky coverage

  5. IFS with Laser Guide Star Adaptive Optics VLT Yepun (UT4) with PARSEC laser Can be used with NACO (imager) and SINFONI (IFU) • High AO resolution also for fainter targets (R~17) w/o extra guidestar • PARSEC running well since 2008

  6. How to weigh a host galaxy • Velocities: narrow emission lines (galaxy) • Dominating: broad lines (AGN) • Need to remove broad lines H HST 3“ SINFONI datacube: all wavelengths coadded

  7. How to weigh a host galaxy [NII] H [NII] +53 km/s –10 km/s –146 km/s • Remove broad H • Trace (narrow) H and [NII] in each spaxel

  8. Result: H velocity field theor. vel. field sketch HST HE0047–1746: enclosed M~6.5•1010 Msun (assuming Kepler) Still needed: velocity field fit including lens model  Inskip, Jahnke, Rix, Peng et al., in prep.

  9. MBH–Mbulge-relation HE0047–1756 (z=1.67) lies off the local M–M-relation (x3–10 in Mgal) Consistent with Peng et al. 2006a+b: „mild evolution at z<1.7“ (Not fully consistent with z=1.3 non-evolution in MBH– Mtot from Jahnke et al. 2009  poster)  Velocity field + lens model fit pending MBH/Msun M*/Msun

  10. Summary & Future • Dynamical H-masses of quasar host galaxies 3/4 the way towards the Big Bang • Prerequisites: IFU, high spatial resolution from Laser AO, large telescope, (GTO time) • We: data for 3 other reduced (1 no H, 1 sky-line blend, 1 promising), 4 new in SINFONI queue for P84 • Collaborators: Keck Osiris IFU spectrograph (two campaigns, no data), retry same targets

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