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AGN Unification in COSMOS

AGN Unification in COSMOS. Jonathan Trump. Chris Impey (Arizona), Martin Elvis, Brandon Kelly, Francesca Civano (CfA), Yoshi Taniguchi, Tohru Nagao (Ehime), Knud Jahnke, Marcella Brusa, Mara Salvato (Max-Planck), Pat McCarthy (Carnegie), Anton Koekemoer (STScI). COSMOS AGN survey.

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AGN Unification in COSMOS

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  1. AGN Unification in COSMOS Jonathan Trump Chris Impey (Arizona), Martin Elvis, Brandon Kelly, Francesca Civano (CfA), Yoshi Taniguchi, Tohru Nagao (Ehime), Knud Jahnke, Marcella Brusa, Mara Salvato (Max-Planck), Pat McCarthy (Carnegie), Anton Koekemoer (STScI)

  2. COSMOS AGN survey • Four years of Magellan/IMACS & MMT/Hectospec spectroscopy over 2 deg2 • 4 magnitudes fainter than SDSS • Type 1 AGN masses from virial scaling relations • Faint and obscured AGNs to z~1 • HST/ACS data for host morphologies to z~1 • Type 2 AGN masses from host-SMBH relations • Complete SEDs • Deep radio, IR, optical, UV, X-ray photometry • Bolometric luminosities • Bolometric luminosity + Mass = Accretion Rate

  3. Accurate bolometric luminosities Model SED as accretion disk + X-ray corona Top: BL Bottom: NL (with host galaxy) Ignore extra reprocessed IR emission

  4. Broad-Line AGN Masses • MBH ~ L0.5 × vfwhm2, scatter of ~0.4 dex • Calibrated from reverberation mapping of ~30 local AGN • Virial theorem: MBH ~ RBLRvBLR2 • RBLR~L0.5 (Kaspi et al. 2000, 07): scaling relations

  5. Masses for Narrow-Line and Lineless AGNs • No broad emission lines... host – MBH relations instead • log(MBH/M⊙) ~ 0.9 log(LK,bulge) − 31 • ~0.35 dex scatter • Bulge luminosities from HST/ACS decompositions (Gabor+09) • Graham 2007

  6. AGN Fueling • LI/LEdd: accretion rate • With Ldisk/LX, Epeak of disk, X-ray slope

  7. AGN Fueling Broad-Line AGN Obscured Narrow-Line AGN Unobscured Narrow-Line & Lineless AGN

  8. AGN Fueling • Broad-line and Obscured Narrow-Line AGN limited by L/LEdd > 0.01

  9. AGN Fueling (unobscured only) • Disk gets brighter & hotter as accretion rate increases (at >3σ significance)

  10. Accretion Rate and Radio Jets • Weakly accreting AGNs are more radio-loud! • Weak AGNs may be important for radio-mode feedback (e.g. heating cluster cores, IGM enrichment)

  11. Accretion Rate and the IR “Torus” • Hot “torus” dust will have IR signature from 1-10μm with αIR<0.5 • Weak AGNs lack this IR signature • Can be explained by disk wind of both BLR & clumpy dust

  12. AGN Fueling • With increasing accretion rate (LI/LEdd)… • Disk luminosity increases compared to X-rays • Disk becomes hotter • Weaker radio outflows • More likely to have IR “torus” signature • Broad emission lines appear (at LI/Ledd>0.01) • Accretion rate is an “axis” of AGN unification • At low accretion rates, theory predicts a radiatively inefficient accretion flow (RIAF) which can produce these effects (Narayan & McClintock 2008)

  13. Accretion in AGN Unification LI/LEdd > 0.01 LI/LEdd < 0.01

  14. Reverberation Mapping • Measure time delay between variability in the broad lines and the continuum • Virial theorem: MBH ~ RBLRvBLR2 • RBLR=ctlag • vBLR=vFWHM • Calibrator for all non-local MBH!!!

  15. Summary • Accretion Rate: new axis in AGN Unification • Low accretion rate: RIAF at inner radii • RIAF: radio-loud, cooler + weaker disk • BLR disappears at L/LEdd < 0.01 • Torus weakens at low accretion rate? • Only possible with COSMOS!!! • Reverberation mapping for more accurate MBH in progress

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