The Relation among Black Holes, Host Galaxies and AGN Activity

1. The Relation among Black Holes, Host Galaxies and AGN Activity Alessandro Marconi INAF-Osservatorio Astrofisico di Arcetri In collaboration with: David Axon, Dan Batcheldor, Andrea Comastri, Roberto Gilli, Günther Hasinger, Leslie Hunt, David Merrit, Roberto Maiolino, Guido Risaliti, Marco Salvati

2. Summary of the talk • The “genesis” of MBH-spheroid scaling relations. • What happens at the high mass end? • Local BHs, AGN relics, and the X-ray background.

3. MBH– host spheroid correlations • MBH- LSph (Kormendy & Richstone 1995, McLure & Dunlop 2002, Marconi & Hunt 2003) • MBH- MSph(Magorrian et al. 1998, Marconi & Hunt 2003, Häring & Rix 2004) • MBH- σe(Ferrarese & Merritt 2000, Gebhardt et al. 2000, Tremaine et al. 2002, Ferrarese & Ford 2005) • MBH-C,n (Concentration or Sersic index, Graham et al. 2001, 2003) • Spheroid structural parameters LSph, σe, Re are tightly related through the fundamental plane, correlations are not independent. • Are correlation slopes AND intrinsic dispersions consistent with the fundamental plane? • Which is the fundamental correlation?

4. MBH is tightly related with virial mass (~σe2 Re; Marconi & Hunt 2003) • Residuals of MBH-σeare weakly dependent on Re (Marconi & Hunt 2003) • There exist correlations with Re and σe4 Re (gravitational energy). • A “fundamental” relation MBH = f(LSph, σe, Re )?

5. The fundamental relation is likely MBH-σ (or any in which the contribution from σ dominates): slopes and dispersions of all other correlations are a consequence of the fundamental plane relation; intrinsic dispersions depend on Δ and are all comparable (Marconi & Hunt 2006, in prep). + observed fundamental plane relation with dispersion ⇒ analytical expressions for slopes and dispersions of MBH-L, MBH-σ, MBH-Mvir as a function of α, β, γ, Δ

6. Problems at the high mass end? • Lauer et al. 2006, Bernardi et al. 2006 find that at the high mass end (BCGs) MBH estimates from σ and from LV or LR are inconsistent: MBH(LV,R) > 1010 M, MBH(σ) < 3╳109 M (e.g., M87) • This “inconsistency” (bending of σ-L relation) have led these authors to speculate that BCGs might form by “dry merging” and that L is the best MBH estimator. • This “inconsistency” would also have important consequences for the high mass end of the BH mass function. Without taking it into account the BHMF would be grossly underestimated (Lauer et al. 2006, Tundo et al. 2006).

7. Problems at the high mass end? • The inconsistency disappears using NIR luminosities (from 2MASS). • Either BCGs have faint extended blue envelopes or L(NIR) is underestimated because 2MASS is missing the faint extended haloes but ... • the agreement between MBH(LJ,H,K)and MBH(σ) is NOT coincidental and means that one should not consider extended envelopes in galaxy scaling relations! • The BHMF does not need any correction! Batcheldor, Marconi, Merrit & Axon, 2006 ApJL, submitted (astro-ph/0610264)

8. Local Black Holes and AGN relics Hard-X LF • Marconi et al. 2004 have shown that local BHs are relics of AGN activity by comparing: • the local BH mass function (from galaxy L/σ functions and MBH-Lbul/MBH-σe) • the relic BHMF (from AGN luminosity function and continuity equation) • Importance of AGN LF: even the hard (2-10 keV) XLF does not sample the whole AGN population. • Heavily obscured Compton-thick AGN are missing ... Soft-X LF Qso LF

9. X-ray Background constraints XRB models provide the total numbers of Compton-thin + Compton-thick AGN. New model by Gilli, Comastri & Hasinger: • Compton-Thin/Unobscured: from comparison of Hard-Soft X-ray LF • Absorbing column density N(H) distribution: from soft and hard X-ray counts. • Compton Thick/Thin: from X-ray background fitting. • Dispersion in AGN continuum slope:reduces by 2xthe number of CT sources • Number of CT sources depends on assumption of 2% scattering efficiency With Compton-thick No Compton-thick Gilli, Comastri, Hasinger 2006, submitted to A&A

10. Local BHMF vs Relic BHMF Hopkins et al. 2006 determine the AGN bolometric luminosity function directly from survey data at mid-IR, optical, and X-ray wavelengths. No substantial change from our results! • Number of Compton-Thick sources from XRB models to consider the whole AGN pop. • The only free parameters are the average accretion efficiency and Eddington ratio • Start with ε=0.1 (L= ε dM/dt c2) λ=1 (L= λ LEdd) ... • and find best ε and λ values.

11. Radiative Efficiency and Fraction of Eddington luminosity • Efficiency and fraction of Eddington luminosity are the only free parameters! • Determine locus in ε-λ plane where there is the best match between local and relic BHMF! • ε=0.04-0.09 λ=0.06-0.4 which are consistent with common ‘beliefs’ on AGNs • Marconi et al. 2004 found using Ueda et al. 2003: ε=0.04-0.16 and λ=0.1-1.7 method is robust!

12. Radiative Efficiency and Fraction of Eddington luminosity • Effect of changing scattering efficiency to compute pure reflection spectra of Compton-Thick sources 2% 0.5% 10%

13. Duty cicle of active BHs • δ is the fraction of Active BHs • δ = Φ(L,t) / N(MBH,t) • In agreement with other independent estimates (Wang et al. 2006)

14. Conclusions • Local correlations of MBH with host spheroid are consistent with being generated by a combination of a fundamental MBH-σ relation and the fundamental plane (Marconi & Hunt 2006, in preparation) • At the high mass end there is no discrepancy between MBH-σ and MBH-L(NIR). One should not consider faint extended galaxy haloes in BH scaling relations. (Batcheldor, Marconi, Merrit, Axon 2006, submitted) • We have updated the analysis of Marconi et al. 2004 taking in to account the most recent and accurate model of the X-ray background as well as other determination of the bolometric AGN luminosity function. The Marconi et al. 2004 results are “robust” and are not substantially changed by these “upgrades”. • Local BH's grew during AGN phases in which accreting matter was converted into radiation with ε = 0.04-0.09 and emitted at a fraction λ = 0.06-0.4 of the Eddington luminosity (Marconi et al. 2006 in preparation)