AGN in Clusters of Galaxies - Berkeley Cosmology Group

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Carnegie: John Mulchaey Dan Kelson Alex Athey Southampton: Christian Kaiser Arizona: Ann Zabludoff Collaborators The Ohio State University: Timothy Arnold Jonathan Bird Jason Eastman Greg Sivakoff Harvard-Smithsonian CfA: Eunhyeuk Kim
Cluster Physics & the Cool Core Problem Clusters of galaxies are filled with hot (T~10 8 K) and diffuse (n~10 -3 cm -3 ) gas The gas in the core should radiatively cool in less than a Hubble time, but not enough cool gas is observed Burns (1990) noted most cool cores harbor powerful AGN Fabian et al. (2005); Schmidt et al. (2002) Perseus
Page 1: AGN in Clusters of Galaxies Paul Ma
Page 5 and 6: Black Hole Evolution Rapid black ho
Page 7 and 8: Galaxy Evolution in Clusters Do the
Page 9: Demographics Berlind et al. (2006)
Page 12 and 13: Mock Catalogs Create a mock catalog
Page 14 and 15: Radio Power at 1.4 GHz [w/Hz/sr] Lu
Page 16 and 17: Fraction of Sources < Projected Jet
Page 18: Distribution of AGN within Clusters
Page 21 and 22: Spectroscopic Confirmation Identifi
Page 23 and 24: AGN Identification LMXBs Hot Gas Jo
Page 25 and 26: Centrally Concentrated AGN Luminous
Page 27 and 28: Centrally Concentrated AGN Implicat
Page 29 and 30: AGN Fraction vs. Environment >95% p
Page 31 and 32: Field AGN Downsizing Silverman et a
Page 33 and 34: AGN in z>0.5 clusters
Page 35 and 36: Comparison to Field AGN More pronou
Page 37: Summary The FRII lifetime is ~10 7

AGN in Clusters of Galaxies - Berkeley Cosmology Group

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