How does AGN Feedback Evolve in Clusters of Galaxies Julie Hlavacek-Larrondo Einstein Fellow,...

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.

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

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

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


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]


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)


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

[email protected]


(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]




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


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

“High/Soft state”Radiatively-efficientShakura & Sunyaev 1973

“Low/Hard state”Radiatively-inefficient

Narayan & Yi 1994, 1995

Quiescent state(e.g. Sgr A*)


1%

0.01%

0.0001%

Lo

g L

nu

cleu

s(2-1

0 keV

)

1 + z


Ed

din

gto

n ratio


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




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

)

Semler et al. 2013

Below z=0.6

Russell et al. 2013

How does AGN Feedback Evolve in Clusters of Galaxies Julie Hlavacek-Larrondo Einstein Fellow,...

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