how does agn feedback evolve in clusters of galaxies julie hlavacek-larrondo einstein fellow,...
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![Page 1: How does AGN Feedback Evolve in Clusters of Galaxies Julie Hlavacek-Larrondo Einstein Fellow, Stanford University Collaborators: Andy Fabian, Steve Allen,](https://reader035.vdocument.in/reader035/viewer/2022070306/5517371f55034603568b5fcf/html5/thumbnails/1.jpg)
How does AGN Feedback Evolve in Clusters of Galaxies
Julie Hlavacek-LarrondoEinstein Fellow, Stanford University
Collaborators: Andy Fabian, Steve Allen, Alastair Edge, Harald Ebeling,Jeremy Sanders, Mike Hogan and Greg Taylor.
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z < 0.3MS0735 (z=0.21), McNamara et al. 2005
200 kpc
?
AGN feedback in Brightest Cluster Galaxies
1) Duty cycle ≥ 95 % in cool core clusters.
2) Energetics are sufficient to prevent the hot gas from cooling.Birzan et al. 2004, Rafferty et al. 2006, Dunn & Fabian 2006, 2008, Dunn
et al. 2010, Birzan et al. 2008, Cavagnolo et al. 2010, Dong et al. 2010…
z > 0.3
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z < 0.3MS0735 (z=0.21), McNamara et al. 2005
200 kpc
AGN feedback in Brightest Cluster Galaxies
1) Duty cycle ≥ 95 % in cool core clusters.
2) Energetics are sufficient to prevent the hot gas from cooling.Birzan et al. 2004, Rafferty et al. 2006, Dunn & Fabian 2006, 2008, Dunn
et al. 2010, Birzan et al. 2008, Cavagnolo et al. 2010, Dong et al. 2010…
Redshift
LX
-ray, cluster (1044
erg/s)
Ebe
ling et al. 2010
Hlavacek-Larrondo et al. 2012
z > 0.3
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Summary of mechanical AGN feedback:1) Duty cycles remain high (>60-95%) in z>0.3 cool core clusters.
2) Energetics are *still* sufficient to prevent the hot gas from cooling.
No significant evolution in mechanical AGN feedback (z=0.0-0.55)
Pcavities [1042 erg
/s]
Lcool ( < rcool ) [1042 erg/s]
Fabian et al. 20
12
Other studies
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Hlavacek-Larrondo et al. 2012
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Light travel time: 3Gyrs 5 Gyrs 8Gyrs
Lo
g L
nu
cleu
s(2-1
0 keV
)
1 + z
32 Massive clusters with X-ray cavities Clusters with “cool cores”/AGN activity
[Santos et al. 2012; Russell et al 2012; Siemiginowska et al. 2012; Iwasawa et al. 2005; McDonald et al. 2012]
AGN feedback in z > 0.3 Brightest Cluster Galaxies
A significant fraction of massive strong cool core clusters at z=1 will host quasars.
Problem for cluster surveys (see also Russell et al. 2012)
Hlavacek-Larrondo et al. 2013
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Conclusion How does AGN feedback evolve in BCGs?
5 Gyrs
1)No significant evolution in mechanical AGN feedback in BCGs (z = 0.0 – 0.55).
1)The nuclear X-ray luminosities of BCGs with X-ray cavities are rapidly evolving: A signifiant fraction will host a quasar by z=1 (i.e. outshine the cluster X-ray emission).
1)Future: SPT, Planck – many new high redshift clusters discovered.
Hlavacek-Larrondo et al. 2012, MNRAS, 421, 1260; Hlavacek-Larrondo et al. 2013, MNRAS accepted, arXiv: 1211.5606
Redshift = 0.0 Redshift = 0.55
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Light travel time: 3Gyrs 5 Gyrs 8Gyrs
(1+z)4
Lo
g L
nu
cleu
s(2-1
0 keV
)
1 + z
Evolution of radiative AGN feedback in BCGs
Evolution of the star formation rate (peaks at z=2-3; e.g. Madau et al. 1996)
32 Massive clusters with X-ray cavities Clusters with “cool cores”/AGN activity
[Santos et al. 2012; Russell et al 2012; Siemiginowska et al. 2012; Iwasawa et al. 2005; McDonald et al. 2012]
Hlavacek-Larrondo et al. 2013
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Evolution of radiative AGN feedback in BCGs
Light travel time: 3Gyrs 5 Gyrs 8Gyrs
Lo
g L
nu
cleu
s(2-1
0 keV
)
1 + z
Number of sources: 32
Fra
ctio
n w
ith a
de
tec
tab
le
X-ra
y n
uc
leu
s
1 + z
Hlavacek-Larrondo et al. 2013
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0.0001% 0.01% 1% 100%
Eddington ratioChurazov et al. 2005
State transition of an « actif » black hole“Thin disk” model(Shakura & Sunyaev 1973)
“Thick disk” model, Advection Dominated Accretion Flow (ADAF; Narayan & Yi 1994)
Pp
ow
er / P
Ed
din
gto
n
0.0001%
0.01%
1
%
100%
Quiescent state (e.g. SgrA*)
High/Soft state
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“High/Soft state”Radiatively-efficientShakura & Sunyaev 1973
“Low/Hard state”Radiatively-inefficient
Narayan & Yi 1994, 1995
Quiescent state(e.g. Sgr A*)
Light travel time: 3Gyrs 5 Gyrs 8Gyrs
1%
0.01%
0.0001%
Lo
g L
nu
cleu
s(2-1
0 keV
)
1 + z
Evolution of radiative AGN feedback in BCGs
Ed
din
gto
n ratio
Hlavacek-Larrondo et al. 2013
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Nu
mb
er
Cooling time (Gyr)
Mechanical duty cycle of BHs in BCGs
≥ 60-95 % of the time.
X-ray cavities + radio
76 MACS clusters at z > 0.3
Nu
mb
er
Cooling time (Gyr)
No X-ray cavities + no radioNo X-ray cavities + radio
Potential X-ray cavities
Clear X-ray cavities
Dunn &
Fab
ian 2006; updated
Cool Core
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Hlavacek-Larrondo et al. 2012
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AGN feedback in z > 0.3 Brightest Cluster Galaxies
MACS J1532.9+3021 (z=0.36; 105 ks)
Lx-ray = 4 *1045 erg/sPcavities = 4 * 1045 erg/s
CL
AS
H: H
ST
F8
14
W (re
d), F
62
5W
(gre
en
), F4
75
W (b
lue
)
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Semler et al. 2013
Below z=0.6
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Russell et al. 2013