AGN feeding and feedback: beyond sub-grid physics Andrea Negrihiddenmonsters/talks/negri.pdf ·...
Transcript of AGN feeding and feedback: beyond sub-grid physics Andrea Negrihiddenmonsters/talks/negri.pdf ·...
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AGN feeding and feedback:beyond sub-grid physics
Andrea Negri
In collaboration with Marta Volonteri
Hidden Monsters: Obscured AGN and Connections to Galaxy EvolutionFriday 12 August 2016
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~last decade: hydro cosmological simulations
dark matter + stars + gas
Evolution of the large scale structure
Andrea Negri – AGN feeding and feedbackIllustris simulation
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~last decade: hydro cosmological simulations
dark matter + stars + gas
Evolution of the large scale structure
Andrea Negri – AGN feeding and feedbackIllustris simulation
Huge dynamical range!currenly impossible to simulate
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~last decade: hydro cosmological simulations
dark matter + stars + gas
Evolution of the large scale structure
Andrea Negri – AGN feeding and feedbackIllustris simulation
Huge dynamical range!currenly impossible to simulate
Simulations are forced to adopt lower resolution
~ 6 kpc for MassiveBlack at z=0 (Di Matteo+2012)
~ 1 kpc for Horizon-AGN (Dubois+2012)
> 750 pc Illustris (10 pc hydro, Vogelsberger+14)350 pc EAGLE simulation, z=0 (Schaye+14)
need to resort to subgrid models for BH accretion
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Subgrid models for BH accretion
Andrea Negri – AGN feeding and feedback
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Subgrid models for BH accretion
Various models are present in literature, most of them based on Bondi Bondi accretion
M BH=α4π G2 M BH
2 ρ
c s3
formal solution of: ● spherically symmetric accretion problem● adiabatic, no feedback, no rotation
Andrea Negri – AGN feeding and feedback
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Subgrid models for BH accretion
Various models are present in literature, most of them based on Bondi Bondi accretion
M BH=α4π G2 M BH
2 ρ
c s3
In simulations we have:● non spherical accretion● multiphase gas● rotation
formal solution of: ● spherically symmetric accretion problem● adiabatic, no feedback, no rotation
Andrea Negri – AGN feeding and feedback
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How accretion is implemented
and cs are calculated using information on the
surrounding gas, plenty of ways (every code/author)
M BH=α4π G2 M BH
2 ρ
c s3
Andrea Negri – AGN feeding and feedback
● Volume weighted (GADGET, Booth+09, Vogelsberger+13)● Mass weighted (Dubois+12)● ISM subgrid model (hot/cold phase, Pelupessy+07)●Global mass w. averages from all the cells (Choi+2012)●Direct accretion of hot and cold gas when hydro is more resolved than gravity (Steinborn+15)
Sometimes it is not even mentioned!
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How accretion is implemented
and cs are calculated using information on the
surrounding gas, plenty of ways (every code/author)
M BH=α4π G2 M BH
2 ρ
c s3
Andrea Negri – AGN feeding and feedback
● Volume weighted (GADGET, Booth+09, Vogelsberger+13)● Mass weighted (Dubois+12)● ISM subgrid model (hot/cold phase, Pelupessy+07)●Global mass w. averages from all the cells (Choi+2012)●Direct accretion of hot and cold gas when hydro is more resolved than gravity (Steinborn+15)
Sometimes it is not even mentioned!
Roughly classified as● MassMass weighted
●Volume Volume weighted (SPH)
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How accretion is implemented
(~100-300) is a boost factor, depends on resolution and sub-grid models of ISM
Andrea Negri – AGN feeding and feedback
M BH=α4π G2 M BH
2 ρ
c s3
● Constant (Springle+05, Dubois+12, Curtis+15)● Depends on ISM density (Booth+09, Steinborn+15)● Depends on feedback (Vogelsberger+13)●Sometimes not used (Pelupessy+07, Choi+12)●Sometimes is not even mentioned!
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How accretion is implemented
(~100-300) is a boost factor, depends on resolution and sub-grid models of ISM
Andrea Negri – AGN feeding and feedback
M BH=α4π G2 M BH
2 ρ
c s3
● Constant (Springle+05, Dubois+12, Curtis+15)● Depends on ISM density (Booth+09, Steinborn+15)● Depends on feedback (Vogelsberger+13)●Sometimes not used (Pelupessy+07, Choi+12)●Sometimes is not even mentioned!
Philosophy behind Low resolution: ISM cold phase not resolved
Bondi radius not resolved●underestimated● c
s overestimated
BH accretion rate underestimatedunderestimated
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Past attempts to calibrate the BH accretion by simulating the Bondi solution
has been performedwithout feedback
Andrea Negri – AGN feeding and feedback
see Wurster+13, Elahi+16
But they used Bondi accretion to simulate Bondi solution!
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Past attempts to calibrate the BH accretion by simulating the Bondi solution
has been performedwithout feedback
Andrea Negri – AGN feeding and feedback
see Wurster+13, Elahi+16
But they used Bondi accretion to simulate Bondi solution!
What happens with feedbackfeedback?
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A simple ideaA simple idea
Sims with same setup but with Bondi accretion:● Different schemes of weighting
●Different resolution
Fiducial simulations comparison with
Andrea Negri – AGN feeding and feedback
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Simulations of an isolated galaxy:
● High resolution ~ 0.1 pc0.1 pc (cold and hot phase)● Well resolvedWell resolved Bondi radius for all the T
● NoNo parametrized accretion
A simple ideaA simple idea
Sims with same setup but with Bondi accretion:● Different schemes of weighting
●Different resolution
Fiducial simulations comparison with
Andrea Negri – AGN feeding and feedback
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Simulations in a nutshell
Code: ZEUSMP (modified in Novak et al. 2011)
●2D axisymmetric
●MBH
= 3 × 107 M ☉
● Rbondi
= 0.1 pc at
T=108 K
●r from 0.1 pc to 250 kpc 0.1 pc to 250 kpc
●Mechanical Feedback Mechanical Feedback from broad absorption line (BAL) winds
● Radiative Radiative feedback
●Compton heating/cooling
●Radiative cooling
Andrea Negri – AGN feeding and feedback
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Simulations in a nutshell
Code: ZEUSMP (modified in Novak et al. 2011)
●2D axisymmetric
●MBH
= 3 × 107 M ☉
● Rbondi
= 0.1 pc at
T=108 K
●r from 0.1 pc to 250 kpc 0.1 pc to 250 kpc
●Mechanical Feedback Mechanical Feedback from broad absorption line (BAL) winds
● Radiative Radiative feedback
●Compton heating/cooling
●Radiative cooling
Andrea Negri – AGN feeding and feedback
fiducial model:fiducial model:BH accretion is fluxflux on the innermost
radial grid
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Andrea Negri – AGN feeding and feedback
cooling – accretion – feedback – hot bubble cycle
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Andrea Negri – AGN feeding and feedback
cooling – accretion – feedback – hot bubble cycle
CHAOTIC ACCRETIONCHAOTIC ACCRETION
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Andrea Negri – AGN feeding and feedback
cooling – accretion – feedback – hot bubble cycle
CHAOTIC ACCRETIONCHAOTIC ACCRETION
Feedback self-limits accretion to sub-Eddington values
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Andrea Negri – AGN feeding and feedback
What happens with Bondi?
1)Define accretion radius racc
2) Calculate and cs inside r
acc
3) no boost factor
Computational grid
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Andrea Negri – AGN feeding and feedback
What happens with Bondi?
1)Define accretion radius racc
2) Calculate and cs inside r
acc
3) no boost factor
Computational grid
● High vs low resolution runs
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Andrea Negri – AGN feeding and feedback
What happens with Bondi?
1)Define accretion radius racc
2) Calculate and cs inside r
acc
3) no boost factor
Computational grid
● High vs low resolution runs● Mass vs Volume weighted
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Andrea Negri – AGN feeding and feedback
Bondi low resolution mass weightedNO AGN
The central resolution is 3, 30 and 300 pc
The expected trend is recoveredin absenceabsence of AGN feedback
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Andrea Negri – AGN feeding and feedback
Bondi low resolutionmass weighted
Explored racc
= 3, 30, 300 pc
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Andrea Negri – AGN feeding and feedback
Trend: the larger rthe larger raccacc the larger the larger MMBHBH!!
Bondi low resolutionmass weighted
Explored racc
= 3, 30, 300 pc
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Andrea Negri – AGN feeding and feedback
Trend: the larger rthe larger raccacc the larger the larger MMBHBH!!
Bondi low resolutionmass weighted
I was expecting the opposite! Why?
Explored racc
= 3, 30, 300 pc
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Sims with large racc
there is a stronger stronger feedback feedback but a
larger gaslarger gas mass to heat/sweep away tostop the accretion
Andrea Negri – AGN feeding and feedback
Bondi high resolution
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Sims with large racc
there is a stronger stronger feedback feedback but a
larger gaslarger gas mass to heat/sweep away tostop the accretion
Andrea Negri – AGN feeding and feedback
Bondi high resolution
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Sims with large racc
there is a stronger stronger feedback feedback but a
larger gaslarger gas mass to heat/sweep away tostop the accretion
Andrea Negri – AGN feeding and feedback
Bondi high resolution
At small racc
the AGN feedback is more effective in stopping the accretion
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Again, at low resolution the AGN feedback isless efficient
Compensates the fact that the accretion is dominated by hot modehot mode
Andrea Negri – AGN feeding and feedback
Bondi low resolutionvolume weighted
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Again, at low resolution the AGN feedback isless efficient
Compensates the fact that the accretion is dominated by hot modehot mode
Andrea Negri – AGN feeding and feedback
Bondi low resolutionvolume weighted
How you calculate density and T mattersmatters!
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Andrea Negri – AGN feeding and feedback
Mass weighted sims
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Andrea Negri – AGN feeding and feedback
Volume weighted sims
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Andrea Negri – AGN feeding and feedback
Take home points● At high resolution high oscillating BH accretion: self-limitedself-limited evolution, kept sub-Eddington without artificial limiters
● The common assumption of low resolution = low accretion is not verified not verified in presence of feedback
● EfficencyEfficency of (mechanical) feedback in stopping accretion is low at low resolutionlow at low resolution
●Accretion boosting Accretion boosting is justified only with volume weighted algorithms (SPH and Illustris simulation) but you need to be very careful!
●alpha is resolution and problem dependant
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Additional slides
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Simulations in a nutshell
Code: ZEUSMP (modified in Novak et al. 2011)
●2D axisymmetric
●Spherical coordinates
●r from 0.1 pc to 250 kpc 0.1 pc to 250 kpc
●NO gas self-gravity (important in 3D)
●SN Ia & SNII
●Mechanical Feedback Mechanical Feedback from broad absorption line (BAL) winds
●Star formation (KS prescription)
●Compton heating/cooling, radiation pressure
●Radiative cooling
Andrea Negri – AGN feeding and feedback
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●Spherical stellar population (Jaffe model) Reff = 5,3 kpc M
star = 3 × 1010 M☉
●BH potential well MBH
=3 × 107 M☉
+ Singular Isothermal Sphere (vc=150 km/s)
●Initial ISM density profile: flat at low r, at large radii r -2
●Two different central ISM density: 1 and 0.01 cm -3
● (Almost) no rotation
Initial conditions
Andrea Negri – AGN feeding and feedback
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●Spherical stellar population (Jaffe model) Reff = 5,3 kpc M
star = 3 × 1010 M☉
●BH potential well MBH
=3 × 107 M☉
+ Singular Isothermal Sphere (vc=150 km/s)
●Initial ISM density profile: flat at low r, at large radii r -2
●Two different central ISM density: 1 and 0.01 cm -3
● (Almost) no rotation
Initial conditions
Andrea Negri – AGN feeding and feedback
MBH
= 3 × 107 M ☉ with 0.1 pc resolution
we are able to resolve the Bondi radius up to T = 108 K
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●Spherical stellar population (Jaffe model) Reff = 5,3 kpc M
star = 3 × 1010 M☉
●BH potential well MBH
=3 × 107 M☉
+ Singular Isothermal Sphere (vc=150 km/s)
●Initial ISM density profile: flat at low r, at large radii r -2
●Two different central ISM density: 1 and 0.01 cm -3
● (Almost) no rotation
Initial conditions
Andrea Negri – AGN feeding and feedback
BH accretion is computed as the fluxflux on the innermost radial grid
MBH
= 3 × 107 M ☉ with 0.1 pc resolution
we are able to resolve the Bondi radius up to T = 108 K