AGN Unification in COSMOS
description
Transcript of AGN Unification in COSMOS
![Page 1: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/1.jpg)
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)
![Page 2: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/2.jpg)
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
![Page 3: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/3.jpg)
Accurate bolometric luminosities
Model SED as accretion disk + X-ray corona
Top: BL
Bottom: NL (with host galaxy)
Ignore extra reprocessed IR emission
![Page 4: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/4.jpg)
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
![Page 5: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/5.jpg)
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
![Page 6: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/6.jpg)
AGN Fueling
• LI/LEdd: accretion rate
• With Ldisk/LX, Epeak of disk, X-ray slope
![Page 7: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/7.jpg)
AGN Fueling
Broad-Line AGNObscured Narrow-Line AGN
Unobscured Narrow-Line & Lineless AGN
![Page 8: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/8.jpg)
AGN Fueling
• Broad-line and Obscured Narrow-Line AGN limited by L/LEdd > 0.01
![Page 9: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/9.jpg)
AGN Fueling (unobscured only)
• Disk gets brighter & hotter as accretion rate increases (at >3σ significance)
![Page 10: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/10.jpg)
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)
![Page 11: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/11.jpg)
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
![Page 12: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/12.jpg)
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)
![Page 13: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/13.jpg)
Accretion in AGN Unification
LI/LEdd < 0.01
LI/LEdd > 0.01
![Page 14: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/14.jpg)
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!!!
![Page 15: AGN Unification in COSMOS](https://reader036.fdocuments.net/reader036/viewer/2022062423/568143f6550346895db080cf/html5/thumbnails/15.jpg)
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