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

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

Introduction n Three categories of astrophysical BHs u Primordial BHs: M~10^15g, not detected yet u Stellar-mass BHs: M~3-20 solar masses, ~20 detected in BH X-ray binaries u Supermassive BHs: M~10^6- 10^9 solar masses, exist in the center of galaxies n Intermediate-mass BHs: M~10^2-10^4 solar masses (??)

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

An example of supermassive BH: M87 M~10 9 M ⊙ Measured by dynamic method

Supermassive BH in the center of our Milky Way M  4x10 6 M 

Reverberation mapping u R BLR estimated by the time delay that corresponds to the light travel time between the continuum source and the line- emitting gas: R BLR =c  t u V estimated by the FWHM of broad emission line Peterson (1997)

Primary Methods: Phenomenon:BL Lac Objects Quiescent Galaxies Type 2 AGNs Type 1 AGNs Summary: Methods of estimating SMBH Masses Stellar, gas dynamics Megamasers2-d RM 1-d RM Fundamental Empirical Relationships: M BH –  * AGN M BH –  * Secondary Mass Indicators: Fundamental plane:  e, r e   *  M BH Broad-line width V & size scaling with luminosity R  L 0.7  M BH Low-z AGNs High-z AGNs [O III ] line width V   *  M BH Peterson (2004)

Analogy between Stellar-mass BH and Supermassive BH systems: Common physics: BH, accretion disk, jet,...

Black Hole Fundamental Plane n BH: Mass (M) n Accretion disk: X-ray emission(L X ) n Jet: Radio emission(L R ) n Any relation among L R, L X 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 n Problem of previous studies u non-uniform samples n Our sample u a uniform radio and X-ray emitting broad line AGN sample selected from SDSS-RASS-FIRST surveys (Wang, Wu & Kong, 2006, ApJ; astro-ph/ ) u including 76 radio-loud and 39 radio-quiet AGNs

Black hole mass estimates n Virial law (Kaspi et al. 2000) n R-L Hβ relation (Wu et al. 2004) n 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 n Differences from previous results u a uniform sample u Different slopes for radio-loud and radio-quiet AGNs u Weak/no dependence on BH mass n Underlying physics u Different X-ray origins: accretion for RQ AGNs; jet for RL AGNs u 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,α r =0.5,α x =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