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How does AGN Feedback Evolve in Clusters of Galaxies

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.

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How does AGN Feedback Evolve in Clusters of Galaxies

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  1. 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.

  2. 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…

  3. AGN feedback in Brightest Cluster Galaxies z < 0.3 z > 0.3 LX-ray, cluster (1044 erg/s) MS0735 (z=0.21), McNamara et al. 2005 Ebeling et al. 2010 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

  4. AGN feedback in z > 0.3 BrightestCluster Galaxies Fabian et al. 2012 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

  5. AGN feedback in z > 0.3 BrightestCluster 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

  6. Conclusion How does AGN feedback evolve in BCGs? juliehl@stanford.edu Redshift = 0.0 Redshift = 0.55 5 Gyrs • No significant evolution in mechanical AGN feedback in BCGs (z = 0.0 – 0.55). • 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). • 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

  7. 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

  8. Evolution of radiative AGN feedback in BCGs Number of sources: 32 Light travel time: 3Gyrs 5 Gyrs 8Gyrs Fraction with a detectable X-ray nucleus Log Lnucleus(2-10 keV) 1 + z 1 + z Hlavacek-Larrondo et al. 2013

  9. State transition of an « actif » black hole “Thin disk” model (Shakura & Sunyaev 1973) “Thick disk” model, Advection Dominated Accretion Flow (ADAF; Narayan & Yi 1994) Ppower / PEddington 0.0001% 0.01% 1% 100% Quiescent state (e.g. SgrA*) High/Soft state 0.0001% 0.01% 1% 100% Eddington ratio Churazov et al. 2005

  10. Evolution of radiative AGN feedback in BCGs Eddington ratio Light travel time: 3Gyrs 5 Gyrs 8Gyrs Log Lnucleus(2-10 keV) “High/Soft state” Radiatively-efficient Shakura & Sunyaev 1973 1% 0.01% 0.0001% “Low/Hard state” Radiatively-inefficient Narayan& Yi 1994, 1995 Quiescent state (e.g. Sgr A*) 1 + z Hlavacek-Larrondo et al. 2013

  11. Dunn & Fabian 2006; updated AGN feedback in z > 0.3 BrightestCluster Galaxies Number Cooling time (Gyr) Cool Core Mechanical duty cycle of BHs in BCGs ≥ 60-95 % of the time. No X-ray cavities + no radio No X-ray cavities + radio X-ray cavities + radio 76 MACS clusters at z > 0.3 Number Clear X-ray cavities Potential X-ray cavities Cooling time (Gyr) Hlavacek-Larrondo et al. 2012

  12. AGN feedback in z > 0.3 BrightestCluster Galaxies CLASH: HST F814W (red), F625W (green), F475W (blue) MACS J1532.9+3021 (z=0.36; 105 ks) Lx-ray = 4 *1045 erg/s Pcavities = 4 * 1045 erg/s

  13. Below z=0.6 Semler et al. 2013

  14. Russell et al. 2013

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