Intrinsic Properties of Quasars:

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Intrinsic Properties of Quasars Testing the
Standard Paradigm
David Turnshek University of Pittsburgh
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• Outline
• Overview
• Models and Constraints
• Emphasis ELR BALR and work with SDSS data
• Model Testing (2.5D ADW Models)
• Recent Collaborators
• Nicholas Pereyra ? modeling and variability
• Kyu-Hyun Chae ? gravitational lens constraints
• Tim Hamilton ? HST imaging
• John Hillier ? modeling
• Norm Murray ? consultant on modeling
• Stan Owocki ? modeling
• Daniel Vanden Berk SDSS collab ? SDSS data

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Overview

• Luminosities (1044 1046 ergs/s) SEDs
• x-ray, UV, optical, IR, (10 radio)
• AGN/QSO Typing ? lots of jargon
• (Sy1, NLSy1, Sy2) (RLQ, RQQ, BAL QSO) (OVV)
• QSO Hosts ? relation to normal galaxies
• Black Hole Mass Measurments
• normal galaxies ? MBH correlated with both
  stellar velocity dispersion and bulge luminosity
• QSOs/AGN ? MBH from (spatially unresolved)
  reverberation size vs. Hb BEL width

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SDSS QSO Colors vs Redshift
Richards et al. 2002
QSO selection colors, x-ray RASS matches, radio
FIRST matches.
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QSO Host Galaxies
Bachall et al HST shows QSO host galaxies are
luminous
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QSO Host Galaxies

• Hamilton, Casertano, Turnshek 2002
  HST observations of 71
  QSOs with zlt0.46

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MBH (Normal Galaxies)
Ferrarese Merritt 2000 Gebhardt et al
2000 Tremaine et al 2002
Magorrian et al 1998 Haring Rix 2004
MBH from spatially resolved velocity measurements
versus stellar velocity dispersion
MBH from spatially resolved velocity
measurements versus bulge mass

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MBH (QSOs/AGN)
Peterson et al 2004

MBH virial mass from (spatially unresolved)
reverberation mapping size scale and Hb velocity
width comparisons with Eddington Luminosity.
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MBH (Normal Galaxies and QSOs/AGN)
McLure Dunlop 2002
Ferrarese et al 2001
MBH versus stellar velocity dispersion

Bulge absolute magnitude versus MBH
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Models and Constraints

• QSOs ?Black Hole Accretion (Lynden-Bell 1969)
• Early Work on ELR and BALR (Cloud Models of the
  BELR)
• Clues from Host Galaxy Type?
• Unified Scenarios vs. Evolutionary Scenarios
• ELR sizes from Reverberation Mapping
• ELR sizes from Gravitational Lensing
• Systematics Constraints from SDSS Spectroscopy

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Models and Constraints

• QSOs ?Black Hole Accretion (Lynden-Bell 1969)
• Early Work on ELR and BALR
• (Cloud Models of the BELR)
• Clues from Host Galaxy Type?
• Unified Scenarios vs. Evolutionary Scenarios

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Models and Constraints

• Early Work (Cloud Models of BELR)
• Absence of OIII BEL
• Presence of CIII BEL
• Baldwin Effect
• Seyfert 1 vs. Seyfert 2 Interpretation
• BAL QSO Interpretation
• No Significant BELs from RLS (e.g. CIV)
• Effect of Dust in BALR?
• Narrow-Line OIII Interpretation

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Basic Early Models Constraints

• Absence of OIII BEL
• ? electron densities gt 105 cm-3
• Presence of CIII BEL
• ? electron densities lt 1011 cm-3
• Baldwin Effect
• ? inverse correlation Luminosity versus BEL REW

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OIII BEL Absent CIII BEL Present
Vanden Berk et al. 2002
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Baldwin Effect
Turnshek 1997
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Models and Constraints

• Early Work (Cloud Models of BELR)
• Absence of OIII BEL
• Presence of CIII BEL
• Baldwin Effect
• Seyfert 1 vs. Seyfert 2 Interpretation
• BAL QSO Interpretation covering factor?
• No Significant BELs from RLS (e.g. CIV)
• Effect of Dust in BALR?
• Narrow-Line OIII Interpretation

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Importance of Viewing Angle

• Seyfert 1 vs. Seyfert 2
• See BELs in polarized (scattered) light of
  Seyfert 2!
• ? obscuring dusty torus (Antonucci Miller 1985)
• ? must have viewing angle effects!

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Importance of Viewing AngleSeyfert 1 vs. Seyfert
2
NGC 4261 Jaffe et al 1993
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Broad Absorption Line QSOs

• BAL QSOs (e.g. Turnshek et al 1980, 84, 85)
• ? viewing angle or evolution?

CIV BEL not due to RLS ? often taken as evidence
that BALR covering factor small But if dust
in BALR? ? could have larger BALR covering factor
(RLS destroys emission)
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Measuring BALR Abundances
Turnshek et al 1996 measure different ions of
the same element ? super solar abundance
(but need to be careful about continuum source
coverage)
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Maybe Viewing Angle IsntAlways Important!

• Narrow-Line OIII Emission
• Emission from this line should be isotropic
• ? but some QSOs have weak OIII (esp. BAL QSOs)
• (Boroson Green 1992, Turnshek et al 1994,
  97) ? suggests that BALR covering factors
  can be large

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Evidence For Intrinsic DifferencesStrong-OIII
vs. Weak-OIII
Boroson 2002
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Models and Constraints

• QSOs ?Black Hole Accretion (Lynden-Bell 1969)
• Early Work on ELR and BALR
• (Cloud Models of the BELR)
• Clues from Host Galaxy Type
• (Do Host Galaxies of BAL QSOs Look Different?) ?
  open question!
• Unified Scenarios vs. Evolutionary Scenarios

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Unified Model for QSOs/AGN
e.g. Elvis 2000
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Unified Model for QSOs/AGN
e.g. Elvis 2000
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Importance of Intrinsic Properties in QSOs/AGN
e.g. Boroson 2002
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Models and Constraints

• ELR sizes from Reverberation Mapping
• (already discussed for black hole mass
  derivations)
• ELR sizes from Gravitational Lensing
• Systematics Constraints from SDSS Spectroscopy

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ELR Sizes Reverberation Mapping
e.g. Peterson et al 2004
?
Peak at 0 days due to noise.
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Models and Constraints

• ELR sizes from Reverberation Mapping
• ELR sizes from Gravitational Lensing
• Systematics Constraints from SDSS Spectroscopy

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ELR Sizes Gravitational Lensing
Cloverleaf QSO Models Chae Turnshek (1999)
contours shown at 40, 80, 160, 320, 640 pc
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ELR Sizes Gravitational Lensing
Narrow-band difference image (Lya minus
continuum)
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Models and Constraints

• ELR sizes from Reverberation Mapping
• ELR sizes from Gravitational Lensing
• Systematics Constraints from SDSS Spectroscopy

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SDSS Results QSO Composite
Vanden Berk et al 2001
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SDSS Results QSO Composite Spectrum
Vanden Berk et al 2001
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SDSS Results EL Velocity Shifts
Vanden Berk et al 2001
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SDSS Results BEL Velocity Shifts
Richards et al 2002
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SDSS Results QSO Types
Reichard et al 2003
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SDSS Results QSO Types
Reichard et al 2003
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SDSS Results Low Ionization BAL QSO
Reichard et al 2003
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SDSS Results Low Ionization BAL QSO
Reichard et al 2003
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SDSS Results BAL Variations
Reichard et al 2003
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SDSS Results QSO PCA
Yip et al 2004
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SDSS Results QSO PCA
Yip et al 2004
PCA benefits Reduce dimensionality Link
diverse (correlated) properties Increase
effective S/N through analysis of large samples
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SDSS Results QSO Galaxy PCA
Yip et al 2004
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Continuum Variability SDSS SpectraA Method to
Measure Black Hole Mass
Pereyra et al 2004
Red flux at minimum Blue flux at maximum
T2Tdisk,max
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Continuum Variability SDSS Spectra
Pereyra et al 2004 Measuring Black Hole Mass
.
DfOl ? Macc
.
(T)4 (Macc/MBH2)
T 2Tdisk,max
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Aside (non-SDSS) Continuum Variability QSO
Type
Sirola et al 1999 Testing Unified Models
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Accretion Disk Wind Models

• Murray et al 1995 1D ADW Model
• Consistent with BALs (x-ray weak), absence of
  double-peaked BELs, reverberation mapping results
• Need for 2.5D
• Proga versus Pereyra see Pereyra et al 2004
• Stability?
• Incorporation of Magnetic Fields?
• 2.5D Model Calculations and Testing

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2.5D ADWModels
Pereyra, Hillier, Murray, Owocki, Turnshek
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2.5D ADWModels
Pereyra, Hillier, Murray, Owocki, Turnshek
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2.5D ADWModels
Pereyra, Hillier, Murray, Owocki, Turnshek
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2.5D ADW Models
Absorbing gas originates from a small range of
radii, rotating tornado-like (BEL widths
comparable to Keplerian velocities, but with
significant outflow component to
velocity). Pereyra, Hillier, Murray, Owocki,
Turnshek
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Broad Absorption Line QSOs

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2.5D ADW Models
BALs flow is quasi-steady outflow. Pereyra,
Hillier, Murray, Owocki, Turnshek
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2.5D ADW Models
Pereyra, Hillier, Murray, Owocki, Turnshek
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2.5D ADW Models
Right disk obscuration at 9000 km/s (units of
inner disk radii deprojected)
Left Q 85o
Pereyra, Hillier, Murray, Owocki, Turnshek
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Conclusions

• Unified Models of QSOs/AGN need to be further
  developed ? they can now be rigorously tested.
• 2.5D Accretion Disk Wind Models (MBH, Macc, )
  offer a good starting point for this.
• The wealth of information from the SDSS database,
  and other observations, offer unprecedented
  opportunities to test QSO/AGN models
• Can we explain the frequency distribution of QSO
  properties (esp. EL velocity shifts BAL types)?
• Can we find a signature of orientation in Radio
  Quiet QSOs?
• Can we find good cases for measurement of metal
  abundances?

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