QUASAR EVOLUTION

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QUASAR EVOLUTION

• Deborah Dultzin-Hacyan
• Instituto De Astronomia (UNAM) México
• Paola Marziani Instituto Nacionale di
  Astrofisica, Osservatorio Astronomico di Padova,
  Italy
• Jack W. Sulentic University of Alabama, USA
• Alenka Negrete Instituto de Astronomia (UNAM)
  México

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• RESULTS FROM REVERBERATION MAPPING OF NGC5548
• (Korista et. al. 1995)
• HST and GROUND MONITORING OF BROAD LINE RESPONSE
  TO UV CONTINUUM VARIATIONS
• HIGH IONIZATION LINES RESPOND WITHIN 2 LIGHT DAYS
  
• (0.0065 Pc)
• LOW IONIZATION LINES RESPOND WITHIN 20 LIGHT DAYS
• (0.065 Pc)
• NARROW LINE REGION IS RESOLVED BY HST 0.3-30 Pc
• BY NOW MORE THAN 30 SEYFERTS HAVE BEEN STUDIED
  THIS WAY
• (Peterson et. al. 2004 Kaspi et. al. 2005
  Collin et al. 2006)
• BLR WILL NOT BE SPATIALY RESOLVED IN THE
• FORSEEABLE FUTURE

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Eigenvectors of Quasars
Quasar spectra are not similar! Historic
inability to explain line ratios via simple
photoionization models
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EIGENVECTOR 1 PARAMETER SPACE
FWHM H? velocity dispersion of LIL EW
(FeII Optical) / EW (Broad H?) (RFeII) ratio
of LIL with opposite density dependences Soft
X-ray Photon Index (?soft) thermal emission
signature CIV ?1549 Broad Line Shift
systematic motions of HIL
Precursors
Boroson Green (1992) Boller et al. (1996)
Marziani et al. (1996) Wang et al.
(1996)Laor et al. (1997)
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Population A FWHM Hß lt 4000Kms-1 Population A
FWHM Hß gt 4000Kms-1
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Pop A B separates in many ways
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FWHM H?
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Black Hole Masses

• H? profile is dominated by gravity. Emitting gas
  is virialized (much observational evidence and
  Susy Collins talk this afternoon)
• H? not available in optical spectra for quasars
  with zgt1
• Some authors have restored to using CIV profiles
  for quasars with zgt1 instead (e.g.Vestergaard
  2002 2004 Dietrich Hamann 2004)
• But there is evidence that CIV emitting gas can
  be dominated by radiation pressure (e.g. Baskin
  Laor 2005) at least for pop A quasars (Bachev et
  al . 2004 Marziani et al. in preparation)
• We have observed 50 quasars in the range 0ltzlt2.5
  with IR spectrometer ISAAC on VLT (25 published
  in Sulentic et al. 2004 2006). S/N 30 in
  continuum

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• CAVEATS and SOURCES OF ERRORS
• see detailed discussion in Sulentic et al. 2006
• Astro-ph/0606309
• 1. Use of single epoch and/or low S/N spectra
• 2. Strongly asymmetric profiles can produce
  uncertainties of up to 40 in Black Hole Masses
  estimated from FWHM H? (Marziani et al. 2003),
  even with high S/N spectra. e.g., no correction
  for VBLR red asymmetric, optically thin (not
  reverberating) component of broad H? (in pop B).
• 3. Lack of proper subtraction or contamination
  of FeII, HeI, broad OIII 4959/5007 and even H
  ?NC
• Orientation effects (Collin et al. 2006
  Astro-ph/0603460) and her talk this afternoon

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We present results from nearly 300 high S/N (30
in continuum) optical spectra from San Pedro
Matir, Mexico and 25 IR spectra from ISAAC on
VLT1 (Antu)

• Each spectrum covers the region of redshifted H?
  and FeII?4570 or FeII?5130
• Ho70 Kms-1Mpc-1, OM0.3, O?0.7, k
  correction computed for a0.6 (S ?a)

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Using corrected FWHM H?
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Lets try FWHM FeII (also virialized Zhang,
Dultzin-Hacyan Wang MNRAS 2006 Astro-ph/0607566)
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Using FWHM FeII
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Now lets look at Eddington ratios
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Correcting face-on RL for orientation
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Correcting face-on NLSy1s for orientation
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CONCLUSIONS

• There seems to be a limit to BH mass evolution
  with z. MBHlt1010M? for masses determined from
  Balmer and FeII emitting gas at low and
  intermediate redshifts
• This is reasonable because, if the dispersion
  velocity - bulge mass - BH mass relation holds
  for intermediate and high z, higher BH masses
  would imply bulge velocity dispersions 700 Kms-1
  and bulge masses 1013 M?

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At Joint Discussion 07 the Universe at z6

• J.D. Kurk reported on recent ISAAC/VLT IR
• spectorscopy of 6 (?) 7 quasars with z5
• BH masses determined from MgII lines (also
• assumed to be emitted from virialized gas) are
  also lt1010
• which CONFIRMS THIS RESULT

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conclusions

• E1 four dimentional diagram may provide a
  surrogate to
• H-R diagram for AGN with L/LEDD and MBH as
  physical underlying parameters. Pop A objects
  show systematically higher L/LEDD and lower MBH
  than pop B objects (including most radio loud
  objects)