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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 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 • 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
Accurate bolometric luminosities Model SED as accretion disk + X-ray corona Top: BL Bottom: NL (with host galaxy) Ignore extra reprocessed IR emission
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
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
AGN Fueling • LI/LEdd: accretion rate • With Ldisk/LX, Epeak of disk, X-ray slope
AGN Fueling Broad-Line AGN Obscured Narrow-Line AGN Unobscured Narrow-Line & Lineless AGN
AGN Fueling • Broad-line and Obscured Narrow-Line AGN limited by L/LEdd > 0.01
AGN Fueling (unobscured only) • Disk gets brighter & hotter as accretion rate increases (at >3σ significance)
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)
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
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)
Accretion in AGN Unification LI/LEdd > 0.01 LI/LEdd < 0.01
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!!!
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