Transcript Julie_Hlavacek

How does AGN Feedback Evolve in
Clusters of Galaxies
Julie Hlavacek-Larrondo
Einstein Fellow, Stanford University
Collaborators: Andy Fabian, Steve Allen, Alastair Edge, Harald Ebeling,
Jeremy Sanders, Mike Hogan and Greg Taylor.
AGN feedback in Brightest Cluster Galaxies
z < 0.3
z > 0.3
MS0735 (z=0.21), McNamara et al. 2005
?
200 kpc
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…
AGN feedback in Brightest Cluster Galaxies
z < 0.3
z > 0.3
MS0735 (z=0.21), McNamara et al. 2005
Ebeling et al. 2010
LX-ray, cluster (1044 erg/s)
200 kpc
Redshift
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…
Hlavacek-Larrondo et al. 2012
bian et al. 2012
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Pcavities [1042 erg/s]
Other studies
Lcool ( < rcool ) [1042 erg/s]
Figure 5: Power inferred from cavities/bubbles plotted against luminosity within the cooling region (where the
radiative cooling time is less than 7 Gyr), courtesy of J. Hlavacek-Larrondo. The objects range from luminous
clusters, through groups, to elliptical galaxies.
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)
Hlavacek-Larrondo et al. 2012
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Light travel time:
3Gyrs
5 Gyrs
8Gyrs
Log Lnucleus(2-10 keV)
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]
 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)
1+z
Hlavacek-Larrondo et al. 2013
[email protected]
Conclusion
How does AGN feedback evolve in BCGs?
Redshift = 0.0
Redshift = 0.55
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
Evolution of radiative AGN feedback in BCGs
Light travel time:
3Gyrs
5 Gyrs
8Gyrs
Log Lnucleus(2-10 keV)
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]
(1+z)4
Evolution of the star formation rate
(peaks at z=2-3; e.g. Madau et al.
1996)
1+z
Hlavacek-Larrondo et al. 2013
Evolution of radiative AGN feedback in BCGs
Light travel time:
3Gyrs
5 Gyrs
Number of sources: 32
8Gyrs
Fraction with a detectable
X-ray nucleus
Log Lnucleus(2-10 keV)
1+z
1+z
Hlavacek-Larrondo et al. 2013
State transition of an « actif » black hole
0.0001%
“Thick disk” model, Advection
Dominated Accretion Flow
(ADAF; Narayan & Yi 1994)
“Thin disk” model
(Shakura & Sunyaev 1973)
Quiescent state
(e.g. SgrA*)
High/Soft state
1%
Ppower / PEddington
0.01%
100%
0.0001%
0.01%
1%
Eddington ratio
Churazov et al. 2005
100%
Evolution of radiative AGN feedback in BCGs
3Gyrs
5 Gyrs
8Gyrs
1%
Log Lnucleus(2-10 keV)
Eddington ratio
Light travel time:
“High/Soft state”
Radiatively-efficient
Shakura & Sunyaev 1973
0.01%
“Low/Hard state”
Radiatively-inefficient
Narayan & Yi 1994, 1995
0.0001%
Quiescent state
(e.g. Sgr A*)
1+z
Hlavacek-Larrondo et al. 2013
n & Fabian 2006; updated
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Cool Core
No X-ray cavities + no radio
No X-ray cavities + radio
X-ray cavities + radio
Mechanical duty cycle
of BHs in BCGs
≥
60-95 % of the time.
Number
76 MACS clusters at z > 0.3
Clear X-ray cavities
Potential X-ray cavities
Cooling time (Gyr)
Number
Cooling time (Gyr)
Hlavacek-Larrondo et al. 2012
ASH: HST F814W (red), F625W (green), F475W (blue)
AGN feedback in z > 0.3 Brightest Cluster Galaxies
Large northern
depression
MACS J1532.9+3021
(z=0.36;
105 ks)
20.0
15.0
Plume
10.0
05.0
30:21:00.0
55.0
50.0
Eastern X-ray cavity
45.0
20:40.0
Western X-ray cavity
35.0
55.5
55.0
Lx-ray = 4 *1045 erg/s
Pcavities = 4 * 1045 erg/s
54.5
15:32:54.0
53.5
53.0
52.5
52.0
Below z=0.6
Semler et al. 2013
Russell et al. 2013