How does AGN Feedback Evolve in Clusters of

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 MS 0735 (z=0. 21), Mc. Namara 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 MS 0735 (z=0. 21), Mc. Namara 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] 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: 3 Gyrs 5 Gyrs 8 Gyrs Log Lnucleus(2 -10 ke. V) 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; Mc. Donald 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

juliehl@stanford. edu 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, ar. Xiv: 1211. 5606

Evolution of radiative AGN feedback in BCGs Light travel time: 3 Gyrs 5 Gyrs 8 Gyrs Log Lnucleus(2 -10 ke. V) 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; Mc. Donald 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: 3 Gyrs 5 Gyrs Number of sources: 32 8 Gyrs Fraction with a detectable X-ray nucleus Log Lnucleus(2 -10 ke. V) 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) Quiescent state (e. g. Sgr. A*) High/Soft state 1% Ppower / PEddington 0. 01% 100% 0. 0001% 0. 01% 1% Eddington ratio Churazov et al. 2005 “Thin disk” model (Shakura & Sunyaev 1973) 100%

Evolution of radiative AGN feedback in BCGs 3 Gyrs 5 Gyrs 8 Gyrs 1% Log Lnucleus(2 -10 ke. V) 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 Number No X-ray cavities + no radio No X-ray cavities + radio Mechanical duty cycle of BHs in BCGs ≥ 60 -95 % of the time. 76 MACS clusters at z > 0. 3 Number Cooling time (Gyr) Clear X-ray cavities Potential X-ray cavities Cooling time (Gyr) Hlavacek-Larrondo et al. 2012

ASH: HST F 814 W (red), F 625 W (green), F 475 W (blue) AGN feedback in z > 0. 3 Brightest Cluster Galaxies MACS J 1532. 9+3021 (z=0. 36; 105 ks) Lx-ray = 4 *1045 erg/s Pcavities = 4 * 1045 erg/s

Below z=0. 6 Semler et al. 2013

Russell et al. 2013