quasar evolution deborah dultzin-hacyan instituto de astronomia (unam) méxico paola marziani...
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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)