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 ~ RBLRvBLR

2

• 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 AGNObscured 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