Xue Xue-Bing Wu- Black Hole Mass and Accretion Rate of Active Galactic Nuclei
Transcript of Xue Xue-Bing Wu- Black Hole Mass and Accretion Rate of Active Galactic Nuclei
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Black Hole Mass andBlack Hole Mass and
Accretion Rate ofAccretion Rate ofActive Galactic NucleiActive Galactic Nuclei
XueXue--Bing Wu (Peking Univ.)Bing Wu (Peking Univ.)[email protected]@bac.pku.edu.cn
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AGN Group in Peking UniversityAGN Group in Peking University
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1. Supermassive Black Holes in Nearby Galaxies
(Kormendy & Richstone 1995; Ho 1999 ; Kormendy
& Gebhardt 2001)
Stellar dynamics
Mass determined by the rotational velocity V
and the velocity dispersion of stars Gas dynamicsKeplerian rotation of ionized gas in a disk-like
configuration Water maser dynamics
22 GHz microwave emission from
extragalactic water masers
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Stellar DynamicsNGC 3115
(Kormendy et al. 1996)M*=2E9 Msun
25 times massiver than
the visible star cluster
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Stellar DynamicsOur Galaxy (Genzel et al. 1997; 2003)
M*=(3~4) E6 Msun
Stellar velocity & proper motionsaround Sgr A* yield a BH mass of(3~4) 106 Msun
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Gas Dynamics Optical emission lines
M87: H, [NII]M*=2.4E9 Msun
Macchetto et al. (1997)
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Water Maser Dynamics Radio masers
22 GHz microwave emission from extragalactic water masersVLBA: resolution 0.0006as
NGC 4258
M*=4E7 Msun
Miyoshi et al. (1995)
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Determination of Supermassive black hole masses inthe center of galaxies (Kormendy & Gebhardt 2001)
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Black hole mass estimations of AGNs
Direct methods
Stellar dynamical studies not feasible in AGN, since
the AGN outshines the stars.
Can use gas kinematics, if the gas is seen in Keplerian
rotation. In M87, r=75 pc gas disk yields 3 109
Msun,>107 Msun pc-3
Megamasers in edge-on nuclear gas disks: Sy2NGC4258, 0.02 pc resolution gives perfect Keplerianrotation (pt mass), 3.6 107 Msun, >5 1012 Msun pc-3
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Indirect Methods Accretion disks fitting of the big blue bump in the
spectra of AGN
Standard thin disk model (Shakura & Sunyaev 1973):
)(1
RdRcos4 11R
R )(/22
3 out
in
= Hzergs
eDc
ihFRkTh
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Accretion disk fitting of the big blue bump in thespectra of AGN (Sun & Malkan 1989)
AD model fits suggest 108-9.5 Msun for quasar, 107.5-8.5 Msun forSy1s, plus mass accretion rates 0.1-1 and 0.01-0.5 times Eddington
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Broad gravitational-redshifted Iron K line ofSeyfert 1 galaxies--accretion disk modeling
Tanaka et al. (1995); Nandra et al. (1997)
Fabian et al. (1989)
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Broad emission line region: 0.01 - 1pc;
Illuminated by the AGN's
photoionizing continuum radiation
and reprocess it into emission lines
RBLR estimated by the time delay that
corresponds to the light travel time
between the continuum source andthe line-emitting gas: RBLR =c t
Vestimated by the FWHM of broad
emission line
GRVM BLR
2
* =
FWHM(H ), 3/2 for random distribution of BLR cloudsV f f= =
Reverberation mapping from optical variability
Peterson (1997)
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Determination of Supermassive black holemasses of AGN with reverberation mapping
Kaspi
et al.
(2000)
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BLR Scaling with LuminosityBLR Scaling with Luminosity
2
HH
24
)H(
rn
L
cnr
QU =
QSOs (Kaspi et al. 2000)
Seyfert 1s (Wandel, Peterson, Malkan 1999) Narrow-line AGNs NGC 4051 (NLS1)
r L0.60.1
To first order, AGN
spectra look the same
Same ionizationparameter
Same density
r L1/2
With the R-L relation, one can estimate the BLR size from theoptical continuum luminosity
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SMBH and Galactic Bulge
Relations of black hole mass with bulge luminosity and central
velocity dispersion (for normal galaxies & AGNs)
Ferrarese et al.
(2001)
AGN
With the M- relation, one can estimate the BH mass from thestellar velocity dispersion
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Summary: Methods of estimating SMBH Masses
PrimaryMethods:
Phenomenon: BL LacObjects
QuiescentGalaxies
Type 2AGNs
Type 1AGNs
Stellar, gasdynamics
Megamasers 2-dRM
1-dRM
FundamentalEmpiricalRelationships:
MBH* AGN
MBH
*
SecondaryMassIndicators:
Fundamentalplane:
e, re * MBH
Broad-line width V& size scaling with
luminosity
R L0.7
MBH
Low-zAGNs
High-zAGNs
[O III] line widthV * MBH
Peterson (2004)
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3. Our progress in AGN BH mass estimations
1. Onblack hole masses, radio loudness and bulge luminosities of Seyfert
galaxies,
Wu & Han 2001, A&A, 380, 31
2. Inclinations andblack hole massesof Seyfert 1 galaxies,
Wu & Han 2001, ApJ, 561, L59
3. Supermassiveblack hole massesof AGNs with elliptical hosts,
Wu, Liu, & Zhang 2002, A&A, 389,7424.Black hole massand binary model for BL Lac object OJ 287,
Liu & Wu 2002, A&A, 388, L48
5.Black hole mass estimation with a relation between the BLR size and
emission line luminosity of AGN,
Wu, Wang, Kong, Liu, & Han 2004, A&A, 424, 793
6.Black hole massand accretion rate of AGNs with double-peaked broad
emission line,Wu & Liu 2004, ApJ, 614, 91
Application of the M- relation
Application of the
fundamental plane relation
Application of the R-L relation
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(1) Estimation of BH masses of(1) Estimation of BH masses of SeyfertSeyfert galaxiesgalaxies
(Wu & Han 2001, A&A, 380, 31)(Wu & Han 2001, A&A, 380, 31)
Sample ofSample ofSeyfertSeyfert galaxiesgalaxies
3737 SeyfertsSeyferts (22(22 SySy 1s, 151s, 15 SySy 2s) with measured M2s) with measured MBHBH oror fromfromtwo brighttwo bright SeyfertSeyfert samplessamples
Palomar: B < 12.5Palomar: B < 12.5 magmag, 49, 49 SeyfertsSeyferts (21(21 SySy 1s, 281s, 28 SySy 2s)2s)
21 Sys selected (1321 Sys selected (13 SySy 1s, 8 Sy2s)1s, 8 Sy2s)
CfACfA:: ZwickyZwicky magnitude
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Sample ofSample ofSeyfertSeyfert galaxiesgalaxies
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Relation of radio powerRelation of radio power
with SMBH masseswith SMBH masses
Correlation between BHCorrelation between BH
mass and bulge magnitudemass and bulge magnitude
MVbulge
= -11.01 -1.22 log (MBH/Msun )=> MBH Mbulge1.74 a non-linear relation
For inactive galaxies
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(2)(2) DetermingDeterming the BLR ithe BLR inclinationnclination ofof SeyfertSeyfert 11
galaxiesgalaxies based on BH mass estimationsbased on BH mass estimations(Wu & Han 2001,(Wu & Han 2001, ApJApJ, 561, L59), 561, L59)
BLR dynamicsBLR dynamics (Wills & Browne 1986)(Wills & Browne 1986)
VirViriial BH massal BH mass
BH massBH mass--velocity dispersion relationvelocity dispersion relation ((GebhardtGebhardt et al.et al.
2000)2000)
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Inclinations of BLR in Seyfert galaxies
Mean value of 36 degree, supporting the AGN unification scheme!
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Inclinations of BLR in Seyfert galaxies
NLS1
Inclination affects the line width; NLS1s seem to have smaller BH masses.
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Woo & Urry, 2002, ApJ, 579, 530 (November); astro-ph/0207249
?
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(3) SMBH Mass of(3) SMBH Mass ofAGNsAGNs with elliptical host galaxywith elliptical host galaxy(Wu, Liu & Zhang, 2002, A&A, 389, 742; August; astro(Wu, Liu & Zhang, 2002, A&A, 389, 742; August; astro--ph/02032158)ph/02032158)
Reverberation mapping can not apply to BLReverberation mapping can not apply to BL LacsLacs; Only 10; Only 10
BLBL LacsLacs have measuredhave measured values (values (FalomoFalomo et al. 2002;et al. 2002; BarthBarthet al. 2002)et al. 2002)
Host galaxies of BLHost galaxies of BL LacsLacs areare ellipticalsellipticals ((UrryUrry et al. 2000)et al. 2000)values can be derived based on thevalues can be derived based on the fundamental planefundamental plane ofofellipticalsellipticals; then SMBH masses could be estimated for BL; then SMBH masses could be estimated for BL
LacsLacswith highwith high--quality imagesquality images
(Bettoni et al. 2001)
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Comparison ofComparison ofEddingtonEddington ratios ofratios ofAGNsAGNs
The Eddington ratios (dimensionless accretion rates) of radio
galaxies are about two orders lower than those of quasars.
( ) l k h l d
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(4) Black hole mass and binary BH
model for BL Lac object OJ 287(Liu & Wu, A&A, 2001, 388, L48)
OJ 287, one of the best studied BL Lacs with optically outburstsrecurrent with a period of 11.65 year (Sillanpaa et al. 1988).
A predicted optical outburst in 1994 was observed and a binary
black hole model is favored (Lehto & Valtonen 1996).
The previous binary BH model requires the primary BH mass
of 1.5E10 solar masses (Pietila 1999), which is much larger than
the estimated BH masses of other BL Lac objects.
A new binary BH model (Valtaoja et al. 2000) with BH mass
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ms
psr
r
(Valtaoja et
al. 2000)
Primary black hole mass of OJ 287:
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Primary black hole mass of OJ 287:
The host galaxy was marginally resolved of an effective radius
re=0.72 and R-band absolute magnitude MR= -23.23 (Heidt et
al. 1999)
Using the BH mass bulge luminosity relation (McLure &Dunlop 2002),
It gives MBH=4.6E8 solar masses.
Using the fundamental plane and the MMBHBH -- relation,
It gives MBH=3.2E8 solar masses.MBH~4E8 solar masses Support the new binary BH model (Valtaoja et al 2000)
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(5) AGN BH Mass estimation with the R-LH relation
(Wu, Wang, Kong, Liu & Han 2004, A&A, 424, 793)
BLR sizes are usually derived previously from the empirical
relation R L5100A0.7(Kaspi et al. 2000). Can it apply to RL AGN? Optical jets of some AGNs have been observed by the HST
(Scarpa et al. 1999; Jester 2003; Parma et al. 2003). Optical
Synchrotron radiations have been found in some RL AGNs
(Whiting et al. 2001; Chiaberge et al. 2002; Cheung et al. 2003)
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For RL AGNs, optical continuum luminosity may be
significantly contributed from jets, and may not be a goodindicator of ionizing luminosity
Using the R-L5100Arelation can overestimate MBH for radio-loudquasars
It may be better to use the relation between the emission lineluminosity and the BLR size
Recently we also extended such a study to UV broad emission lines
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Recently we also extended such a study to UV broad emission lines
(Mg II & CIV) (Kong, Wu, Wang, & Han, 2006)
(6) Black hole mass and accretion rate of AGNs with
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( )
double-peaked broad emission line
(Wu & Liu, 2004, ApJ, 614, 91)
DoubleDouble--peaked broad linepeaked broad line AGNsAGNs are usually believed to beare usually believed to be
LINERLINER--type lowtype low--luminosity ones (Ho et al. 2001)luminosity ones (Ho et al. 2001)
150 double150 double--peaked AGN discovered (SDSS and RLAGN); SDSSpeaked AGN discovered (SDSS and RLAGN); SDSS
doubledouble--peakedpeaked AGNsAGNs: 76% are radio: 76% are radio--quiet, with mediumquiet, with medium
luminosities (1E44 erg/s); 12% are LINER (luminosities (1E44 erg/s); 12% are LINER (StratevaStrateva et al. 2003)et al. 2003)
With the RWith the R--L relation, we estimated the BH mass (from 3E7 toL relation, we estimated the BH mass (from 3E7 to5E9 solar masses) and the5E9 solar masses) and the EddingtonEddington ratio (from 0.001 to 0.1) ofratio (from 0.001 to 0.1) of
135 double135 double--peakedpeaked AGNsAGNs..
We found big blue bumps in some luminous doubleWe found big blue bumps in some luminous double--peakedpeaked AGNsAGNs We suggested that for luminous doubleWe suggested that for luminous double--peakedpeaked AGNsAGNs withwith
EddingtonEddington ratio larger than 0.01, the accretion process is probablyratio larger than 0.01, the accretion process is probably
different from that of LINERdifferent from that of LINER--type doubletype double--peakedpeaked AGNsAGNs
Black hole mass and accretion rate of AGNs with
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Black hole mass and accretion rate of AGNs with
double-peaked broad emission line
5 S d Di i
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5. Summary and Discussion
Supermassive black holes with mass of 106 to 109
solar masses exist in the center of both normal and
active galaxies
Direct dynamic methods of estimating the BH mass
can only be applied to several nearby AGNs. ReliableBH mass of AGNs can be obtained by reverberation
mapping, MMBHBH -- relation (including the fundamentalplane) and two R-L relations.
Estimating the BH mass is important and helpful to
other AGN studies
Eddington ratio and accretion physics in
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Eddington ratio and accretion physics indifferent types of AGN
From the BH mass, we can derive Eddington ratio ( Lbol/Ledd),
which measures the accretion rate in Eddington unit.
Accretion disk structure is strongly dependent on the accretion
rate
SD: Slim disk (Abramowicz et al. 1988)
RTD, GTD: Radiation pressure and
gas pressure dominated thin disk
(Shakura-Sunyaev 1973)SLE: Hot, two-temperature disk
(Shapiro, Lightman & Eardley
1976)
ADAF: Advection dominated accretion
flow (Narayan & Yi 1994)
Abramowicz et al. (1995)
T i i f diff i d
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Transition of different accretion modes as
accretion rate changesApplications in black hole X-ray binaries: (AGN too?)
Fender (2003)
Knowing accretion rate may help us to understand
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Knowing accretion rate may help us to understandthe broad line region physics of AGN
(Nicastro et al.
2003)
A fundamental plane of black hole activity
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A fundamental plane of black hole activity
(Merloni et al. MNRAS, 2003)
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SMBH in highest redshift quasar (z=6 4)
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SMBH in highest redshift quasar (z=6.4)
Supermassive black hole formed in the early universe!Willott et al. (2003) (UKIRT/UIST) Barth et al. (2003) (Keck II/NIRSPEC)
FWHM(MgII)=5500km/sMBH=2E9 Msun
FWHM(CIV)=9000km/sMBH=6E9 MsunFWHM(MgII)=6000km/sMBH=3E9 Msun
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Rees flowchart for theformation of a
very massiveblack hole
Rees (1984)
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Have fun withblack holes !
Thankyou !
Variations of broad line componentVariations of broad line component
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pp
at different luminosity levelat different luminosity level
Kong, Wu, Wang,et al. (2006)
Broad line
component of
CIV line of
NGC 4151
L
BH fundamental plane from a uniform sampleBH fundamental plane from a uniform sample
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p pp p
of radio and Xof radio and X--ray emitting broad lineray emitting broad line AGNsAGNs
Cross-identified RASS-SDSS-FIRST broad line AGNs
Different slope between radio-quiet and radio-loud AGNs
Beaming effect from the relativistic jet of RL AGNs can
contaminate the intrinsic BH fundamental plane relation
Yuan & Cui (2005)Wang, Wu & Kong (2006)