Growth of SMBH: the connection between accretion physics and Cosmology

Growth of SMBH:the connection between accretion physics and Cosmology Andrea Merloni Max-Planck Institute for Astrophysics PASBH – Santa Fe11/07/2006

Intro: Key (observational) questions • What is the mass density of SMBH locally (Richstone, Marconi)? • Constraints on accretion efficiency via Soltan-type arguments • What is the redshift and luminosity distribution of Compton-thick sources (from CXRB ~20-60% effect, Fabian, Marconi)? • Observed correlations (M-, Magorrian): How do they evolve athigh redshift (Shields; Merloni, Rudnick and Di Matteo 2004)? • Constraints on structure formation/feedabck models • What is the evolution of AGN LF? • Evolution of SMBH/host galaxy mass function • What is the Kinetic Luminosity function of AGN, and how does it evolve?

(z=0) = 1.0 Fixed MBH/Mbulge ratio at all z (z=0) = 0.3 MBH/Mbulge increases with redshift Fixed Mbulge/Mdisk+irr ratio at all z Merloni, Rudnick, Di Matteo 2004

Radiative efficiency constraints 1

Parallel lives

Intro: Key (observational) questions • What is the mass density of SMBH locally (Richstone, Marconi)? • Constraints on accretion efficiency via Soltan-type arguments • What is the redshift and luminosity distribution of Compton-thick sources (from CXRB ~20-60% effect, Fabian, Marconi)? • Observed correlations (M-, Magorrian): How do they evolve at high redshift (Shields; Merloni, Rudnick and Di Matteo 2004)? • Constraints on structure formation/feedabck models • What is the evolution of AGN LF? • Evolution of SMBH/host galaxy mass function • What is the Kinetic Luminosity function of AGN, and how does it evolve?

Open questions in accretion theory • Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005, Merloni, Heinz and Di Matteo 2003)Þ jets/outflows dominate over radiation as power sinks. But is radiative efficiency low with respect to the accreted mass (“Are BH green ?” Blandford)? • Advection vs. Outflows (see Gallo et al. 2006 on A0620-00 in quiescence) • What is the physics of Radio-Loud high accretion rate systems (QSOs)? • What fraction of the power do the jet carry? • How common they are (lifetime of the radio active phase)?

Open questions in accretion theory • Low accretion rate systems: X-ray radio correlation in binaries (Gallo et al. 2003, Fender 2005, Merloni, Heinz and Di Matteo 2003)Þ jets/outflows dominate as power sinks. But is radiative efficiency low with respect to the accreted mass (“Are BH green?” Blandford) • Advection vs. Outflows (see Gallo et al. 2006 on A0620-00 in quiescence) • What is the physics of Radio-Loud high accretion rate systems (QSOs)? • What fraction of the power do the jet carry? • How common are they (lifetime of the radio active phase)?

A strategy...(Merloni 2004; Schwab, Heinz & Merloni 2006; Merloni et al. 2006) • Use the Radio-Mass-X-ray (or any other) correlation to break the degeneracy between mass and Eddington ratio for any given Lbol • Use accretion theory(-ies) to estimate accretion rate onto the black hole and kinetic energy output for any given LR-LX-MBH combination • Solve continuity equations for BH growth (Small and Blandford 1992; Marconi et al. 2004) backwards in time, using the locally determined BH MF as a starting point

SMBH downsizing Mass function evolution Merloni (2004)

A strategy...(Merloni 2004; Schwab, Heinz & Merloni 2006; Merloni et al. 2006) • Use the Radio-Mass-X-ray (or any other) correlation to break the degeneracy between mass and Eddington ratio for any given Lbol • Use accretion theory(-ies) to estimate accretion rate onto the black hole and kinetic energy output for any given LR-LX-MBH combination • Solve continuity equations for BH growth (Small & Blandford 1992; Marconi et al. 2004)backwards in time, using the locally determined BH MF as a starting point

Accretion theory in a nutshell (Blandford & Begelmann)

Accretion theory in a nutshell

A strategy...(Merloni 2004; Schwab, Heinz & Merloni 2006; Merloni et al. 2006) • Use the Radio-Mass-X-ray (or any other) correlation to break the degeneracy between mass and Eddington ratio for any given Lbol • Use accretion theory(-ies) to estimate accretion rate onto the black hole and kinetic energy output for any given LR-LX-MBH combination • Solvecontinuity equations for BH growth(Small & Blandford 1992; Marconi et al. 2004)backwards in time, using the locally determined BH MF as a starting point

Kinetic Energy output and feedback history (Lbol/LEdd)crit=0.02; Outflows

Kinetic Energy output and feedback history

Kinetic Energy output and feedback history RLQSO ADIOS/LLAGN

SMBH growth: Energy budget • Fraction of local BH rest mass energy density accumulated in various regimes (multiply by 0.06<η<0.42 to get absolute efficiency of each) • Radiatively efficient RQQSO/AGN~62% • RLQSO~9% (half (?) of which K.E. dominated) • K. E. dominated LLAGN~29% Input/test of cosmological simulations

Conclusions • Comparing the evolution of SMBH and stellar mass densities it is already possible constrain the evolution of the Magorrian relation, using SMBH as tracers. For a given host spheroid mass, BH were more massive at higher redshift.At z=3 we predict <MBH>/<Msph> ~ 2.5 times larger than the local value (Merloni, Rudnick and Di Matteo 2004) • The redshift evolution of SMBH mass, accretion rate and kinetic energy output function can be determined from the joint evolution of X-ray and Radio AGN luminosity functionsusingthe mass-LX-LR relationship • The largest black holes are the first to enter the radiatively inefficient accretion regime. The K.E. feedback from LLAGN jets starts dominating high mass objects first and then objects of progressively lower mass • Kinetic energy output of LLAGN has the right redshift dependence to explain high of galaxy luminosity function(Croton et al. 2006)

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Growth of SMBH: the connection between accretion physics and Cosmology