M BH - σ relation in AGNs
description
Transcript of M BH - σ relation in AGNs
MBH-σ relation in AGNs
Bian WeihaoBian Weihao
Department of Physics, Department of Physics, Nanjing Normal UniversityNanjing Normal University
Outline
1. SMBH masses in AGNs, M1. SMBH masses in AGNs, MBHBH 2. Bulge velocity dispersion,2. Bulge velocity dispersion,σσ3. M3. MBHBH--σσrelation in AGNsrelation in AGNs
~10 17 cm
(Francis et al. 1991)
(Elvis et al. 1994)
1. SMBH masses in AGNs, M1. SMBH masses in AGNs, MBHBH
mvmv2 2 – GmM– GmMBHBH /R = 0 /R = 0
SMBH virial massSMBH virial mass
MBHm
MBH = v2 R /G
Schwarzschild radius: RS = 2GMBH/c2 =3MBH/Msun km
= 3 × 1013 M8 cm=10-2 M8 lt-days.
Period: 15.6 years•R~2000 Rg •(Belgeman, 2003, Science, 300, 1898)
M: (3-4)x106Msun
For S14: R~1000 Rg
Smaller R, Stronger evidence
S2
Virial EstimatorsVirial Estimators
X-Ray Fe K 3-10 RS
Broad-Line Region 103 RS
Megamasers 104 RS
Gas 106 RS
Stellar 106 RS
Reverberation Mapping Techniqueis independent of angular resolution
photoionization model: ionization source variance => emission line variancetime delay
t1 – t2 =
t = t1
t = t2
t = t3
t = t3 +
NGC 5548: RBLR~20 lt-days (~300 days)MBH~108Msun
dtt )()()( ACFCCF
For Quasar PG 0804+761: RBLR~156 lt-days (~6 Years)
(Kaspi, et al. 2000, ApJ, 533,631)
RMS and mean spectrum
Mainly from NLRsBoroson, 2003, ApJ, 585, 647Peterson et al., 2004, ApJ, 613, 282
Peterson et al., 2004, ApJ, 613, 282 HeII4686
PG 1700
• To first order, AGN spectra look the same
• Baldwin EffectBaldwin Effect– C IV C IV 1549, et al.1549, et al.– Origin?Origin?
SDSS compositesVanden Berk et al. astro-ph/0310840
2HH
24
)H(
rn
L
cnr
QU
Same ionization
parameter Same density
r L1/2
RBLR – L scaling relation
To first order, To first order, quasar spectra quasar spectra look similar at look similar at all redshiftsall redshifts
744 Type I AGNs, 0< z< 5;Dietrich et al 2002, ApJ, 581, 912
Vestergaard & Peterson 2006 astro-ph/0601303
M ergs/s10
)1350(λL
km/s10
FWHM(CIV)105.4M
53.0
44λ
2
36
BH
McLure & Jarvis, 2002, MNRAS, 337, 109
Kaspi, et al. 2000, ApJ, 533,631Kaspi et al. 2005, ApJ, 629, 61
M ergs/s
)(λL
km/s10
β)FWHM(H M λ
3BH
0.50
44
26
10
5100108.3
days-lt 100680
42080381
1010
..
Hβ..BLR ergs/s
LR
Wu X., et al., A&A, 2004, 424, 793
MBH=f VFWHMRBLR2/G
f=5.5 \pm 1.8
MBH-σrelation Onken et al., 2004, ApJ, 615, 645
(H0=70 km/s/Mpc; ΩΛ = 0.7)
The slope of RThe slope of RBLRBLR-L relation-L relation
• Host galaxy light iHost galaxy light in Seyfert 1, the lun Seyfert 1, the luminosity at the faiminosity at the faint end.nt end.
• 0.67 => 0.520.67 => 0.52
Bentz et al., 2006, astro-ph/0602412 Bian et al., 2004, ChJAA, 4, 61
problem(dex)
Accuracy
Reverberation 0.3 Zero-point, understand BLR f,
Mapping
Scaling Relations 0.5-0.6 R-L relationships, understand outliers
MBH - relation: -- *
bulge 0.3 Extend to luminous quasars
-- [OIII] [OII] [SII] 0.7 Understand scatter & outliers
-- Fundamental ? Quantify & establish higher Plane: e, re accuracy
MBH – Lbulge 0.6-0.7 Calibrate to reverberation mapped & scaling relations
Kauffmann et al. 2003, MNRAS, 346, 1055Host galaxies of 22623 SDSS AGNs (Type II)
Opt/IR spectra of host galaxies => σCa II triplet 8498 、 8542 、 8662\AA;Mg b triplet 5167 、 5172 、 5183\AA; Ca K+H 3934 3969 \AA
2. Bulge velocity dispersion,2. Bulge velocity dispersion,σσ
Vanden Berk, et al., 2006, AJ, 131, 84, SDSS AGNs, astro-ph/0509332
• Fourier techniques: cross-correlation; Fourier quotient; Fourier correlation quoti
ent• Direct-fitting in pixel space: stellar templates broadened by with σ
σ measurement
g(n): host galaxy spectrum; t(n): template spectrum; B(n-δ): Gaussian broadening functionX: cross-correlation *: convolution
Rix & Whittle, 1992, MNRAS, 254, 389Nelson & Whittle, ApJS, 1995, 99, 67Kauffmann et al. 2003, MNRAS, 346, 1055Cid Fernandes, et al., 2005, MNRAS, 358, 363Greene & Ho, ApJ, 2005,astro-ph/0512462Woo, et al., 2006, ApJ, astro-ph/0603648
t(x): template spectrum G(x): Gaussian broadening functionC(x): AGNs continuum, power-lawP(x): polynomial factor
Nelson & Whittle, ApJS, 1995, 99, 67McElory , 1995, ApJS, 100, 105Kauffmann et al. 2003, MNRAS, 346, 1055Ferrarese, et al. ApJ, 555 ,L79Falomo et al., ApJ, 569, L35Barth, et al., 2005, ApJ, 619, L151, 0412575Greene & Ho, ApJ,2006, astro-ph/0512462Woo, et al., 2006, ApJ, astro-ph/0603648
σ [O III] = FWHM([O III])/2.35σ - σ [O III] relation
• Line asymmetries
• Outflows• Radio sources (jet)
• Interacting systems
Bian, Gu, Zhao, 2006, for 0.3< z 0.83 Type II AGNs SDSS J150117.96+545518.2
3. M3. MBHBH--σσ relation in AGNsrelation in AGNs
Onken, et al., ApJ, 2004, 615, 245 Mass from reverberation mapping method is reliable.
AGNs
Nelson, 2001, ApJ, 544, L91σ[O III] = FWHM([O III])/2.35
Barth, et al., 2005, ApJ, 619, L151, 0412575 Keck II telescope
Greene Ho, ApJL, In press, astro-ph/0512461, 40+16 SDSS AGNs
02.4;13.8
Woo, et al., 2006, ApJ, astro-ph/0603648, Z=0.36
MMBHBH--σσ relation in NLS1srelation in NLS1s
150 NLS1s from SDSS EDR (Williams R.J., Pogge R.W., Mathur S, 2003, AJ, 124, 3042)22 NLS1s from HST observation
(Constantin & Shields, 2003, PASP, 115, 592)
Bian & Zhao, MNRAS, 2004, 347, 607; Grupe & Mathur, 2004, ApJ, 606, L41;Botte, 2005, MNRAS, 356, 789Barth, et al., 2005, ApJ, 619, L151Zhou et al., 2006, astro-ph/0603759, ~308 σ ,for a sample of ~2000 NLS1s from SDSS DR3
Dynamics of NLRs in NLS1s would be different than that of other AGN
Barth, et al., 2005, ApJ, 619, L151,Astro-ph/0412575
NLS1s ??~Z, L5100, L/LEdd
Theory on MTheory on MBHBH – –σσrelationrelation
• Vittorini, Shankar, & Cavalier 2005, astro-ph/0508640Vittorini, Shankar, & Cavalier 2005, astro-ph/0508640 (BH gro (BH growth history from merger/feedback events; simulation)wth history from merger/feedback events; simulation)
• Robertson et al. 2005, astro-ph/0506038Robertson et al. 2005, astro-ph/0506038 (mergers simulation) (mergers simulation)• Di Matteo, Springel, & Hernquist 2005, Nature, 433, 604Di Matteo, Springel, & Hernquist 2005, Nature, 433, 604 (merg (merg
er induced BH growth and starformation; simulation)er induced BH growth and starformation; simulation)• Springel, Di Matteo, & Hernquist 2005, MNRAS, 361, 776Springel, Di Matteo, & Hernquist 2005, MNRAS, 361, 776 (BH/s (BH/s
tar formation feedback; simulations)tar formation feedback; simulations)• Miralda-Escude & Kollmeier 2005, ApJ 619, 30Miralda-Escude & Kollmeier 2005, ApJ 619, 30 (stellar captur (stellar captur
e)e)• Sazonov et al. 2005, MNRAS 358, 168Sazonov et al. 2005, MNRAS 358, 168 (radiative BH feedback) (radiative BH feedback)• King 2003, ApJ 596, L27King 2003, ApJ 596, L27 (supercritical accretion, outflows) (supercritical accretion, outflows)• Adams et al. 2003, ApJ 591, 125Adams et al. 2003, ApJ 591, 125 (rotating BH collapse model) (rotating BH collapse model)• …….and many more…...and many more…..
Thank you !Thank you !