The Fundamental Plane of Astrophysical Black Holes WU Xue-Bing (Peking University) Collaborators: WANG Ran (PKU) KONG Minzhi (NAOC)

The Fundamental Plane of Astrophysical Black Holes

WU Xue-Bing

(Peking University)

Collaborators: WANG Ran (PKU)

KONG Minzhi (NAOC)

Content Introduction: BHs in the universe BH Fundamental Plane Test with a uniform sample Discussions

Introduction Three categories of astrophysical BHs

Primordial BHs: M~10^15g, not detected yet

Stellar-mass BHs: M~3-20 solar masses, ~20 detected in BH X-ray binaries

Supermassive BHs: M~10^6-10^9 solar masses, exist in the center of galaxies

Intermediate-mass BHs: M~10^2-10^4 solar masses (??)

2

33

)1(

sin)(

2 q

iMMf

G

KPX

Xoptorb

An Example of Stellar-mass BH: Cyg X-1

Mass function:

2

3

( )(1 / )

sins x

x

f M M MM

i

Cyg X-1

An example of supermassive BH: M87

M~109 M⊙

Measured by dynamic method

Supermassive BH in the center of our Milky WaySupermassive BH in the center of our Milky WayM M 4x10 4x1066 M M

Reverberation mapping

RBLR estimated by the time delay that corresponds to the light travel time between the continuum source and the line-emitting gas: RBLR =c t

V estimated by the FWHM of broad emission line

Peterson (1997)

G

RVM BLR

2

*

PrimaryMethods:

Phenomenon: BL LacObjects

QuiescentGalaxies

Type 2AGNs

Type 1AGNs

Summary: Methods of estimating SMBH Masses

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-z AGNs

High-z AGNs

[O III] line widthV * MBH

Peterson (2004)

Analogy between Stellar-mass BH and Supermassive BH systems:

Common physics: BH, accretion disk, jet, ...

Black Hole Fundamental Plane BH: Mass (M) Accretion disk: X-ray

emission(LX)

Jet: Radio emission(LR)

Any relation among LR, LX and M?

A fundamental plane of black hole activity

(Merloni, Heinz, & Di Matteo, 2003, MNRAS)

Stellar-mass BHs

Supermassive BHs

Unification scheme for accreting BH systems and radio--X-ray correlation

(Falcke, Kording, & Markoff, 2004, A&A)

Test with a uniform sample Problem of previous studies

non-uniform samples Our sample

a uniform radio and X-ray emitting broad line AGN sample selected from SDSS-RASS-FIRST surveys

(Wang, Wu & Kong, 2006, ApJ; astro-ph/0603514)

including 76 radio-loud and 39 radio-quiet AGNs

Black hole mass estimates

Virial law (Kaspi et al. 2000)

R-LHβrelation (Wu et al. 2004)

McLure -Jarvis (2002) relation

For radio-quiet sources: Different slopes

No correlation with M

The correlation is not dominated by distance & mass

Difference between radio-loud and radio-quiet AGNs in the radio--X-ray relation

The contribution of relativistic beaming effect in radio-loud AGNs

δLog Lr=Log Lr-Log Lr (predict)

Discussions

Differences from previous results a uniform sample Different slopes for radio-loud and

radio-quiet AGNs Weak/no dependence on BH mass

Underlying physics Different X-ray origins: accretion

for RQ AGNs; jet for RL AGNs Relativistic beaming in RL AGNs

Heinz (2004, MNRAS)

Scaling relations for scale-invariant cooled jets (both Lr & Lx are from jets):

For canonical synchrotron spectrum of p=2,αr=0.5,αx=1

Consistent with our results for radio-loud AGNs!

Radio--X-ray correlation with different X-ray origins

(Yuan & Cui 2005, ApJ)

Consistent with the results obtained with our uniform sample!

Flat slopeSteep slope