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How does AGN Feedback Evolve in Clusters of Galaxies Julie Hlavacek-Larrondo Einstein Fellow, Stanford University Collaborators: Andy Fabian, Steve Allen,

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Presentation on theme: "How does AGN Feedback Evolve in Clusters of Galaxies Julie Hlavacek-Larrondo Einstein Fellow, Stanford University Collaborators: Andy Fabian, Steve Allen,"— Presentation transcript:

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 z < 0.3 MS0735 (z=0.21), McNamara et al 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

3 z < 0.3 MS0735 (z=0.21), McNamara et al 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 L X-ray, cluster (10 44 erg/s) Ebeling et al Hlavacek-Larrondo et al z > 0.3

4 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= ) P cavities [10 42 erg/s] L cool ( < r cool ) [10 42 erg/s] Fabian et al Other studies AGN feedback in z > 0.3 Brightest Cluster Galaxies Hlavacek-Larrondo et al. 2012

5 Light travel time: 3Gyrs 5 Gyrs 8Gyrs Log L nucleus (2-10 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

6 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: Redshift = 0.0Redshift = 0.55

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8 Light travel time: 3Gyrs 5 Gyrs8Gyrs (1+z) 4 Log L nucleus (2-10 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

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

10 0.0001% 0.01% 1% 100% Eddington ratio Churazov et al State transition of an « actif » black hole Thin disk model (Shakura & Sunyaev 1973) Thick disk model, Advection Dominated Accretion Flow (ADAF; Narayan & Yi 1994) P power / P Eddington % 0.01% 1% 100% Quiescent state (e.g. SgrA*) High/Soft state

11 Radiatively-efficient Shakura & Sunyaev 1973 Low/Hard state Radiatively-inefficient Narayan & Yi 1994, 1995 Quiescent state (e.g. Sgr A*) Light travel time: 3Gyrs 5 Gyrs8Gyrs 1% 0.01% % Log L nucleus (2-10 keV) 1 + z Evolution of radiative AGN feedback in BCGs Eddington ratio Hlavacek-Larrondo et al. 2013

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

13 AGN feedback in z > 0.3 Brightest Cluster Galaxies MACS J (z=0.36; 105 ks) L x-ray = 4 *10 45 erg/s P cavities = 4 * erg/s CLASH: HST F814W (red), F625W (green), F475W (blue)

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17 Semler et al Below z=0.6

18 Russell et al. 2013


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