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Intrinsic Properties of Quasars: Testing the Standard Paradigm

Intrinsic Properties of Quasars: Testing the Standard Paradigm. David Turnshek University of Pittsburgh. Outline: Overview Models and Constraints Emphasis: ELR + BALR and work with SDSS data Model Testing (2.5D ADW Models) Recent Collaborators:

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Intrinsic Properties of Quasars: Testing the Standard Paradigm

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  1. Intrinsic Properties of Quasars: Testing the Standard Paradigm David Turnshek University of Pittsburgh

  2. 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

  3. 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

  4. SDSS QSO Colors vs Redshift Richards et al. 2002: QSO selection: colors, x-ray RASS matches, radio FIRST matches.

  5. QSO Host Galaxies Bachall et al: HST shows QSO host galaxies are luminous

  6. QSO Host Galaxies • Hamilton, Casertano, Turnshek 2002: HST observations of 71 QSOs with z<0.46

  7. 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

  8. 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.

  9. MBH (Normal Galaxies and QSOs/AGN) Ferrarese et al 2001: McLure & Dunlop 2002: MBH versus stellar velocity dispersion Bulge absolute magnitude versus MBH

  10. 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

  11. 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

  12. 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

  13. Basic Early Models Constraints • Absence of [OIII] BEL •  electron densities > 105 cm-3 • Presence of CIII] BEL •  electron densities < 1011 cm-3 • Baldwin Effect •  inverse correlation: Luminosity versus BEL REW

  14. [OIII] BEL Absent – CIII] BEL Present Vanden Berk et al. 2002:

  15. Baldwin Effect Turnshek 1997:

  16. 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

  17. 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!

  18. Importance of Viewing AngleSeyfert 1 vs. Seyfert 2 NGC 4261: Jaffe et al 1993

  19. 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)

  20. 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)

  21. Maybe Viewing Angle Isn’tAlways 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

  22. Evidence For Intrinsic DifferencesStrong-[OIII] vs. Weak-[OIII] Boroson 2002:

  23. 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

  24. Unified Model for QSOs/AGN e.g. Elvis 2000:

  25. Unified Model for QSOs/AGN e.g. Elvis 2000:

  26. Importance of Intrinsic Properties in QSOs/AGN e.g. Boroson 2002:

  27. 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

  28. ELR Sizes: Reverberation Mapping e.g. Peterson et al 2004:  Peak at 0 days due to noise.

  29. Models and Constraints • ELR sizes from Reverberation Mapping • ELR sizes from Gravitational Lensing • Systematics + Constraints from SDSS Spectroscopy

  30. ELR Sizes: Gravitational Lensing Cloverleaf QSO Models: Chae & Turnshek (1999) contours shown at: 40, 80, 160, 320, 640 pc

  31. ELR Sizes: Gravitational Lensing Narrow-band difference image (Lya – minus continuum)

  32. Models and Constraints • ELR sizes from Reverberation Mapping • ELR sizes from Gravitational Lensing • Systematics + Constraints from SDSS Spectroscopy

  33. SDSS Results – QSO Composite Vanden Berk et al 2001:

  34. SDSS Results – QSO Composite Spectrum Vanden Berk et al 2001:

  35. SDSS Results – EL Velocity Shifts Vanden Berk et al 2001:

  36. SDSS Results – BEL Velocity Shifts Richards et al 2002:

  37. SDSS Results – QSO “Types” Reichard et al 2003:

  38. SDSS Results – QSO “Types” Reichard et al 2003:

  39. SDSS Results – Low Ionization BAL QSO Reichard et al 2003:

  40. SDSS Results – Low Ionization BAL QSO Reichard et al 2003:

  41. SDSS Results – BAL Variations Reichard et al 2003:

  42. SDSS Results – QSO PCA Yip et al 2004:

  43. 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

  44. SDSS Results – QSO & Galaxy PCA Yip et al 2004:

  45. Continuum Variability – SDSS Spectra:A Method to Measure Black Hole Mass Pereyra et al 2004: Red: flux at minimum Blue: flux at maximum T*~2Tdisk,max

  46. Continuum Variability – SDSS Spectra Pereyra et al 2004: Measuring Black Hole Mass . DfOl  Macc . (T*)4 ~ (Macc/MBH2) T* ~ 2Tdisk,max

  47. Aside (non-SDSS): Continuum Variability – QSO Type Sirola et al 1999: Testing Unified Models

  48. 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

  49. 2.5D ADWModels Pereyra, Hillier, Murray, Owocki, Turnshek

  50. 2.5D ADWModels Pereyra, Hillier, Murray, Owocki, Turnshek

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