Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

Black hole mass and cluster mass relation in cosmological hydro-dynamical simulations

Collaborators: S. Borgani, E. Rasia, C. Ragone-Figueroa, V. Biffi, K. Dolag, G.L. Granato, M. Gaspari, G. Murante, G. Taffoni, L. Tornatore

Goals of our work:

✦ Do we reproduce the observed relation?

✦ How the correlation forms?

✦ Through which channel do SMBHs grow in time?

✦ Is as appropriate as BCG mass as proxy for ?

Luigi Bassini (University of Trieste, INAF/OATs)

MBH �M500

MBH �M500

M500 MBH

Arxiv:1903.03142

Luigi Bassini, University of Trieste EUCLID & BEYOND 12/02/2019

7.5

8

8.5

9

9.5

10

10.5

11

10.5 11 11.5 12 12.5

log

MBH

(Msu

n)

log Mbulge (Msun)

BGG/BCG sampleMcconnell & Ma 2013

7.5

8

8.5

9

9.5

10

10.5

11

1 10

log

MBH

(Msu

n)

kT (keV)

BH masses dynamically measured

Temperature obtained from Xray observations

Bulge masses given by Kormendy & Ho 2013

(compilation of different sources)

Bogdan et al. 2018

� = 0.38

� = 0.61

SMBH mass-Galaxy Cluster properties correlations

(See also Phipps et al. 2019 and Gaspari et al. 2019)

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

Numerical set-up and sample selection (Dianoga set)

29 Cosmological hydrodynamical zoom-in simulations extracted from a parent N-body

simulation of 1.4 Gpc side

Simulations performed with the Lagrangian GADGET-3 SPH code (see Beck et al. 2016)

mass resolution: mDM = 8.47⇥ 108h�1M�

mgas = 1.53⇥ 108h�1M�

At z=0 we consider all 135 clusters with:

Subgrid models: radiative cooling, star formation and associated feedback, metal

enrichment and chemical evolution, BH accretion and AGN feedback.

M500 > 1.4⇥ 1013M�

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

Numerical set-up and sample selection(AGN feedback)

Mbondi,↵ = ↵4⇡G2M2

BH⇢

(c2s + v2BH)3/2

✏f = 0.1

✏r = 0.07

✏r = 0.07

✏f = 0.7

↵ = 100 for T < 5⇥ 10

5K↵ = 10 for T > 5⇥ 10

5K

BHs seeded with initial mass of in halos of mass

4.4⇥ 105M�

Radiated fraction

Fraction thermally coupled

quasar mode

radio mode

·Mbondi,α / ·Medd > 0.01

·Mbondi,α / ·Medd < 0.01

·Eth = ϵfϵr·Mbondi,αc2

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

Comparison between numerical results and observations

Numerical results in agreement with observations on the

plane

Scatter around relation lower in numerical simulations

MBH � T500

MBH �MBCG

Calibration of AGN feedback

1011 1012

M? [M�]

108

109

1010

1011

MB

H[M

�]

McConnell & Ma 2013 fit mixed sampleBogdan 2018Gaspari et al. 2019

100 101

T500 [keV]

108

109

1010

1011

MB

H[M

�]

SimulationsBogdan et al. 2018Gaspari et al. 2019σ = 0.14 ± 0.01

σ = 0.16 ± 0.02

M87

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

Establishment of correlation

(1) Rapid growth for

gas accretion

MBH �M500

1012 1013 1014 1015 1016

M500 [M�]

108

109

1010

1011

MB

H[M

�]

Time= 13.91

Sample z=0.0

(2) Structures enter R500

(M500 grows for mergers)

(3) Structures reach the center

(BH grows for gas accretion

and merger)

(M500 grew by more than 40% in the last Gyr)

Systems right after a cluster merger

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

SMBHs mass evolution during cosmic time

0 2 4 6 8 10 12

Time [Gyr]

0.0

0.2

0.4

0.6

0.8

1.0

MBH

(z)/

MBH

(z=

0)

MBH

MaccBH

MmerBH

5 4 3 2 1 0.5z

At z>2 BHs gain mass via gas accretion. Gas is accreted at

the Eddington limit;

At z<2 gas accretion slows down with an accretion rate

which is a fraction of the Eddington limit;

At z<1 BH-BH mergers are the main channel for SMBH mass

growth;

At z=0 the two component equally contribute to the

total mass of SMBHs

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

1013 1014 1015

M500 [M�]

108

109

1010

1011

Mac

cBH

,Mm

erBH

[M�]

MaccBH

MmerBH

1013 1014 1015 1016

M500 [M�]

108

109

1010

1011

Mac

cBH

,Mm

erBH

[M�]

MaccBH

MmerBH

SMBHs mass evolution during cosmic time

z=1

MaccBH

z=0

MmerBH

MaccBH > Mmer

BH

MmerBH ∼ 33 %

MmerBH > Macc

BH

MmerBH ∼ 60 %

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

SMBHs mass evolution during cosmic time

1010 1011 1012 1013

M? [M�]

108

109

1010

1011

M•

[M�]

N = 01 < N 44 < N 10N > 10

Mergers important for the most massive

objects

M∙ ∼ 5 × 107 M⊙ : < N > = 0

M∙ ∼ 5 × 108 M⊙ : < N > = 2

M∙ ∼ 5 × 109 M⊙ : < N > = 4

N number of mergers with M1 : M2 > 0.25

Gaspari et al. 2019

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

SMBHs mass evolution during cosmic time

0

2

4

6

8

10

12

13.5

Tim

e[G

yr]

107

108

M•[M

�]

0

2

4

6

8

10

12

13.5

Tim

e[G

yr]

107

108

M•[M

�]

0

2

4

6

8

10

12

13.5

Tim

e[G

yr]

107

108

M•[M

�]

0

2

4

6

8

10

12

13.5

Tim

e[G

yr]

107

108

109

1010

M•[M

�]

M• ⇠ 108 M• ⇠ 108.5

M• ⇠ 109 M• ⇠ 1010

Luigi Bassini, University of Trieste SMBHs: Environment and Evolution 20/06/2019

✦Once on the relation, systems evolve as a stairway (structures enter grows move towards the center grows via 2 channels)

Conclusions

✦ Simulations reproduce the observed relation between MBH and T500 (M500);

✦ At z>2 BH mass grows by rapid gas accretion and systems set on the relation;

✦ is as reliable as for mass estimate (the scatter of the 2 relations are

comparable)

R500 M500

MBH

MBH �M500 MBH �MBCG MBH

Arxiv:1903.03142