Growth of SMBH: the connection between accretion physics and Cosmology

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Growth of SMBHthe connection between accretion
physics and Cosmology
Andrea Merloni Max-Planck Institute for
Astrophysics
PASBH Santa Fe 11/07/2006
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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?

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MBH/Mbulge increases with redshift
Fixed Mbulge/Mdiskirr ratio at all z
Merloni, Rudnick, Di Matteo 2004
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Radiative efficiency constraints
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Parallel lives
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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?

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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)?

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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)?

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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

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Mass function evolution
Merloni (2004)
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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

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Accretion theory in a nutshell
(Blandford Begelmann)
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Accretion theory in a nutshell
(Blandford Begelmann)
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Accretion theory in a nutshell
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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

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Kinetic Energy output and feedback history
(Lbol/LEdd)crit0.02 Outflows
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
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Kinetic Energy output and feedback history
RLQSO
ADIOS/LLAGN
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SMBH growth Energy budget

• Fraction of local BH rest mass energy density
  accumulated in various regimes (multiply by
  0.06lt?lt0.42 to get absolute efficiency of each)
• Radiatively efficient RQQSO/AGN62
• RLQSO9 (half (?) of which K.E. dominated)
• K. E. dominated LLAGN29
• Input/test of cosmological simulations

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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 z3 we
  predict ltMBHgt/ltMsphgt 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 functions using the
  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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THE END