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The Fundamental Plane of Astrophysical Black Holes

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. I ntroduction.

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The Fundamental Plane of Astrophysical Black Holes

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

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

  3. Introduction • Threecategories 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 (??)

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

  5. An example of supermassive BH:M87 M~109M⊙ Measured by dynamic method

  6. Supermassive BH in the center of our Milky Way • M  4x106 M

  7. Reverberation mapping Peterson (1997) • 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 estimatedby the FWHM of broad emission line

  8. Type 2 AGNs Type 1 AGNs Phenomenon: BL Lac Objects Quiescent Galaxies Primary Methods: Stellar, gas dynamics Megamasers 2-d RM 1-d RM Fundamental Empirical Relationships: MBH– * AGNMBH– * Secondary Mass Indicators: Fundamental plane: e, re  * MBH [O III] line width V  * MBH Broad-line width V & size scaling with luminosity R  L0.7 MBH Summary: Methods of estimating SMBH Masses Low-z AGNs Peterson (2004) High-z AGNs

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

  10. Black Hole Fundamental Plane • BH: Mass (M) • Accretion disk: X-ray emission(LX) • Jet: Radio emission(LR) • Any relation among LR, LX and M?

  11. A fundamental plane of black hole activity (Merloni, Heinz, & Di Matteo, 2003, MNRAS) Supermassive BHs Stellar-mass BHs

  12. Unification scheme for accreting BH systems and radio--X-ray correlation (Falcke, Kording, & Markoff, 2004, A&A)

  13. 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

  14. Black hole mass estimates • Virial law (Kaspi et al. 2000) • R-LHβrelation (Wu et al. 2004) • McLure -Jarvis (2002) relation

  15. No correlation with M Different slopes For radio-quiet sources:

  16. The correlation is not dominated by distance & mass

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

  18. The contribution of relativistic beaming effect in radio-loud AGNs δLog Lr=Log Lr-Log Lr (predict)

  19. 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

  20. 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!

  21. Radio--X-ray correlation with different X-ray origins (Yuan & Cui 2005, ApJ) Steep slope Flat slope Consistent with the results obtained with our uniform sample!

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