Another Cosmological Constant to Solve More Problems of Our Cosmological Model
Black hole mass and cluster mass relation in cosmological ...xraygroup.astro.noa.gr ›...
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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
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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
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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
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10
12
13.5
Tim
e[G
yr]
107
108
M•[M
�]
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Tim
e[G
yr]
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M•[M
�]
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Tim
e[G
yr]
107
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M•[M
�]
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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