M BH - σ relation in AGNs

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M BH -σ relation in AGNs Bian Weihao Bian Weihao Department of Physics, Department of Physics, Nanjing Normal University Nanjing Normal University

description

Bian Weihao Department of Physics, Nanjing Normal University. M BH - σ relation in AGNs. Outline. 1. SMBH masses in AGNs, M BH 2. Bulge velocity dispersion, σ 3. M BH - σ relation in AGNs. 1. SMBH masses in AGNs, M BH. ~10 17 cm. (Elvis et al. 1994). (Francis et al. 1991). - PowerPoint PPT Presentation

Transcript of M BH - σ relation in AGNs

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MBH-σ relation in AGNs

Bian WeihaoBian Weihao

Department of Physics, Department of Physics, Nanjing Normal UniversityNanjing Normal University

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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

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~10 17 cm

(Francis et al. 1991)

(Elvis et al. 1994)

1. SMBH masses in AGNs, M1. SMBH masses in AGNs, MBHBH

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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.

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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

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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 +

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NGC 5548: RBLR~20 lt-days (~300 days)MBH~108Msun

dtt )()()( ACFCCF

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For Quasar PG 0804+761: RBLR~156 lt-days (~6 Years)

(Kaspi, et al. 2000, ApJ, 533,631)

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RMS and mean spectrum

Mainly from NLRsBoroson, 2003, ApJ, 585, 647Peterson et al., 2004, ApJ, 613, 282

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Peterson et al., 2004, ApJ, 613, 282 HeII4686

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PG 1700

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• 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

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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

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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)

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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

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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

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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

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Vanden Berk, et al., 2006, AJ, 131, 84, SDSS AGNs, astro-ph/0509332

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• 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

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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

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Bian, Gu, Zhao, 2006, for 0.3< z 0.83 Type II AGNs SDSS J150117.96+545518.2

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3. M3. MBHBH--σσ relation in AGNsrelation in AGNs

Onken, et al., ApJ, 2004, 615, 245 Mass from reverberation mapping method is reliable.

AGNs

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Nelson, 2001, ApJ, 544, L91σ[O III] = FWHM([O III])/2.35

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Barth, et al., 2005, ApJ, 619, L151, 0412575 Keck II telescope

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Greene Ho, ApJL, In press, astro-ph/0512461, 40+16 SDSS AGNs

02.4;13.8

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Woo, et al., 2006, ApJ, astro-ph/0603648, Z=0.36

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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)

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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

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Barth, et al., 2005, ApJ, 619, L151,Astro-ph/0412575

NLS1s ??~Z, L5100, L/LEdd

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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…..

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Thank you !Thank you !