QUASAR EVOLUTIONQUASAR EVOLUTION

Deborah Dultzin-HacyanDeborah Dultzin-Hacyan Instituto De Astronomia (UNAM) MéxicoInstituto De Astronomia (UNAM) México

Paola MarzianiPaola Marziani Instituto Nacionale di Astrofisica, Instituto Nacionale di Astrofisica, Osservatorio Astronomico di Padova, ItalyOsservatorio Astronomico di Padova, Italy

Jack W. SulenticJack W. Sulentic University of Alabama, USAUniversity of Alabama, USA

Alenka Negrete Alenka Negrete Instituto de Astronomia (UNAM) Instituto de Astronomia (UNAM)

MéxicoMéxico

RESULTS FROM REVERBERATION MAPPING OF NGC5548RESULTS FROM REVERBERATION MAPPING OF NGC5548(Korista et. al. 1995)(Korista et. al. 1995)

HST and GROUND MONITORING OF BROAD LINE RESPONSE TO HST and GROUND MONITORING OF BROAD LINE RESPONSE TO UV CONTINUUM VARIATIONSUV CONTINUUM VARIATIONS

HIGH IONIZATION LINES RESPOND WITHIN 2 LIGHT DAYS HIGH IONIZATION LINES RESPOND WITHIN 2 LIGHT DAYS (0.0065 Pc)(0.0065 Pc)

LOW IONIZATION LINES RESPOND WITHIN 20 LIGHT DAYSLOW IONIZATION LINES RESPOND WITHIN 20 LIGHT DAYS(0.065 Pc)(0.065 Pc)

NARROW LINE REGION IS RESOLVED BY HST 0.3-30 Pc NARROW LINE REGION IS RESOLVED BY HST 0.3-30 Pc

BY NOW MORE THAN 30 SEYFERTS HAVE BEEN STUDIED THIS BY NOW MORE THAN 30 SEYFERTS HAVE BEEN STUDIED THIS WAYWAY

(Peterson et. al. 2004; Kaspi et. al. 2005; Collin et al. 2006)(Peterson et. al. 2004; Kaspi et. al. 2005; Collin et al. 2006)

BLR WILL NOT BE SPATIALY RESOLVED IN THE BLR WILL NOT BE SPATIALY RESOLVED IN THE FORSEEABLE FUTUREFORSEEABLE FUTURE

Averange Quasar Spectrum: Francis et al. 1991

Eigenvectors of Quasars

Quasar spectra are not similar!

Historic inability to explain line ratios via simple photoionization models

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)

Population A: FWHM HPopulation A: FWHM Hββ < 4000Kms < 4000Kms-1-1

Population A: FWHM HPopulation A: FWHM Hββ > 4000Kms > 4000Kms-1-1

RFeII

FW

HM

H

B

A

FWHM H 4000 km/s

Pop Pop A – B separates in many waysA – B separates in many ways

FW

HM

H

RFeII

CIV

no systematic

shift

(high EW)

systematic blueshift

(low EW)

Black Hole MassesBlack Hole MassesHH profile is dominated by gravity. profile is dominated by gravity. Emitting gas is Emitting gas is

virialized (much observational evidence and Susy Collin’s talk virialized (much observational evidence and Susy Collin’s talk this afternoon)this afternoon)

HH not available in optical spectra for quasars with z>1 not available in optical spectra for quasars with z>1Some authors have restored to using CIV profiles for quasars Some authors have restored to using CIV profiles for quasars

with z>1 instead (e.g.Vestergaard 2002; 2004; Dietrich & with z>1 instead (e.g.Vestergaard 2002; 2004; Dietrich & Hamann 2004)Hamann 2004)

ButBut there is evidence that there is evidence that CIV emitting gas can be CIV emitting gas can be dominated by radiation pressuredominated by radiation pressure (e.g. Baskin & Laor (e.g. Baskin & Laor 2005) at least 2005) at least forfor pop A quasarspop A quasars (Bachev et al . 2004; (Bachev et al . 2004; Marziani et al. in preparation) Marziani et al. in preparation)

We have observed 50 quasars in the range We have observed 50 quasars in the range 0<z<2.5 with IR spectrometer ISAAC on VLT0<z<2.5 with IR spectrometer ISAAC on VLT (25 (25 published in Sulentic et al. 2004; 2006). published in Sulentic et al. 2004; 2006). S/N S/N ~30 in ~30 in continuumcontinuum

CAVEATS and SOURCES OF ERRORSCAVEATS and SOURCES OF ERRORS see detailed discussion in Sulentic et al. 2006see detailed discussion in Sulentic et al. 2006

Astro-ph/0606309 Astro-ph/0606309

1. Use of single epoch and/or low S/N spectra 1. Use of single epoch and/or low S/N spectra 2. Strongly asymmetric profiles can produce 2. Strongly asymmetric profiles can produce

uncertainties of up to 40% in Black Hole Masses uncertainties of up to 40% in Black Hole Masses estimated from FWHM Hestimated from FWHM H (Marziani et al. 2003), (Marziani et al. 2003), even with high S/N spectra. e.g., no correction for even with high S/N spectra. e.g., no correction for VBLR red asymmetric, optically thin (not VBLR red asymmetric, optically thin (not reverberating) component of broad Hreverberating) component of broad H (in pop B). (in pop B).

3. Lack of proper subtraction or contamination of 3. Lack of proper subtraction or contamination of FeII, HeI, broad [OIII] 4959/5007 and even H FeII, HeI, broad [OIII] 4959/5007 and even H NCNC

Orientation effects (Collin et al. 2006 Orientation effects (Collin et al. 2006 Astro-ph/0603460) and her talk this afternoonAstro-ph/0603460) and her talk this afternoon

We present results from nearly 300 We present results from nearly 300 high S/N (high S/N (~30 in continuum) ~30 in continuum) optical optical

spectra from San Pedro Matir, Mexico spectra from San Pedro Matir, Mexico and 25 and 25 IR spectra from ISAAC on IR spectra from ISAAC on

VLT1 (AntuVLT1 (Antu)) Each spectrum covers the region of Each spectrum covers the region of

redshifted redshifted HH and FeII and FeIIλλ4570 or 4570 or

FeIIFeIIλλ51305130HHoo=70 Kms=70 Kms-1-1MpcMpc-1-1, , ΩΩMM=0.3, =0.3, ΩΩΛΛ=0.7, k =0.7, k

correction computed for correction computed for αα=0.6 (S =0.6 (S ~~υυαα))

Using corrected FWHM H

Let’s try FWHM FeII (also virialized: Zhang, Dultzin-Hacyan & Wang MNRAS 2006 Astro-

ph/0607566)

Using FWHM FeII

Now let’s look at Eddington ratios

Correcting face-on RL

for orientation

Correcting face-on

NLSy1’s

for orientation

CONCLUSIONSCONCLUSIONS

There seems to be a There seems to be a limit to BH masslimit to BH mass evolution with z. evolution with z. MMBHBH<<10101010MM for for masses determined from Balmer masses determined from Balmer and FeII emitting gas at low and and FeII emitting gas at low and intermediate redshiftsintermediate redshifts

This is reasonable because, if the This is reasonable because, if the

dispersion velocity - bulge mass - BH mass dispersion velocity - bulge mass - BH mass relation holds for intermediate and high z, relation holds for intermediate and high z, higher BH masses would imply bulge higher BH masses would imply bulge velocity dispersions ≥700 Kmsvelocity dispersions ≥700 Kms-1-1 and bulge and bulge masses ≥10masses ≥1013 13 MM

At At Joint Discussion 07 Joint Discussion 07 “the Universe at z“the Universe at z≥6”≥6”

J.D. Kurk reported on recent ISAAC/VLT IRJ.D. Kurk reported on recent ISAAC/VLT IR

spectorscopy of 6 (?) 7 quasars with spectorscopy of 6 (?) 7 quasars with z≥5z≥5

BH masses determined from BH masses determined from MgIIMgII lines (also lines (also

assumed to be emitted from virialized gas) assumed to be emitted from virialized gas) are also are also <<101010 10

which which CONFIRMS THIS RESULTCONFIRMS THIS RESULT

conclusionsconclusions

E1 four dimentional diagram may E1 four dimentional diagram may provide a surrogate to provide a surrogate to

H-R diagram for AGN H-R diagram for AGN withwith L/LL/LEDD EDD and Mand MBHBH as physical underlying as physical underlying parameters. Pop A objects show parameters. Pop A objects show systematically higher L/Lsystematically higher L/LEDD EDD and and lower Mlower MBHBH than pop B objects than pop B objects (including most radio loud objects)(including most radio loud objects)