high-redshift quasars in cosmological...
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High-redshift Quasars in Cosmological Simulations
Colin DeGrafCosmology at the Beach
January 16, 2012
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Outline
● Overview of MassiveBlack simulation● High-z Quasar populations
● Quasar Luminosity Function● Clustering
● Black hole growth rates
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MassiveBlack Simulation
● 533 h-1 Mpc GADGET3 SPH simulation
● BHs seeded at 5*105 h-1 MO
● Grow by mergers and gas accretion
● 5% of radiated energy couples as thermal feedback
● Complete z=4.75 volume viewable at Gigapan● Smaller (50 h-1 Mpc) box evolution available at
Gigapan Time MachineVisualizations created by Yu Feng
MBH=4 πG2 M BH
2ρ
(cs2+vrel
2)
3 /2 LBH=ηM BH c2
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Quasar Luminosity Function
●Bolometric Luminosity Function direct from simulation
DeGraf et al. 2011
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Quasar Luminosity Function
●Bolometric Luminosity Function direct from simulation●Z=5 data compiled by Hopkins et al. 2007
DeGraf et al. 2011
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Quasar Luminosity Function
●Bolometric Luminosity Function direct from simulation●Z=6 data compiled by Hopkins et al. 2007, Willot et al. 2010
DeGraf et al. 2011
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Quasar Luminosity Function - HOD
●Bolometric Luminosity Function direct from simulation●Compared with predicted QLF from redshift-independent HOD●Good agreement, except for bright QSOs at z=6-7
DeGraf et al. 2011
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Quasar Luminosity Function - Predictions
JWST LSST DES VIKING
DeGraf et al. 2011
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Quasar Clustering Evolution
DeGraf et al. 2011
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Black Hole Growth Rates
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Sample Growth Histories
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General growth histories● 25 most massive BHs in our simulation●Growth generally suppressed by 109
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Modeling growth rate
DeGraf et al. in prep
λ=MBH
M edd
=LBH
Ledd
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Modeling growth rate
DeGraf et al. in prep
λ=MBH
M edd
=LBH
Ledd
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Local Gas Density
Suppressed Eddington ratio caused by suppression in local gas density
DeGraf et al. in prep
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Modeling growth rate
DeGraf et al. in prep
λ=MBH
M edd
=LBH
Ledd
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Eddington Ratio Distribution with MBH
P(λ
|MB
H)
P(λ
|MB
H)
P(λ
|MB
H)
P(λ
|MB
H)
λ λ
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Eddington Ratio Distribution with MBH
P(λ
|MB
H)
P(λ
|MB
H)
P(λ
|MB
H)
λ
λ
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Eddington Ratio Distribution with LBH
P(λ
|LB
H)
P(λ
|LB
H)
P(λ
|LB
H)
P(λ
|LB
H)
LBH
=1.1*1011L
BH=2.7*1011
LBH
=6.4*1011 LBH
=1.2*1012
λ λ
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Conclusions
● Simulation provides large statistical sample of quasars for z>4.75
● Evolution in QLF primarily caused by evolution in halo mass function
● Clustering is luminosity-dependent, particularly among brightest QSOs
● QSO Eddington ratios log-normally distributed about (MBH
, z)-dependent mean
● Massive BHs tend to have lower LBH
/Ledd
than less massive
– Suppression caused by BH-feedback on nearby gas
● This typical growth well-characterized by a simple fitted model
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Extra Slides
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Correlation Length
●Correlation length calculated using maximum likelihood estimator
DeGraf et al. 2011
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Correlation Length
●Correlation length calculated using maximum likelihood estimator●Compared to predicted r0 using HOD model
DeGraf et al. 2011
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Predicted luminosity dependence
Assume constant HOD (reasonable to z~3)
DeGraf et al. 2011
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