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AGN in Clusters of Galaxies

AGN in Clusters of Galaxies. Paul Martini The Ohio State University. J.S. Mulchaey, D.D. Kelson (OCIW). E. Kim (CfA), A. Athey (OCIW). Why Survey Clusters for AGN?. Why is this a MISST?. 1. Different environment to probe AGN fueling (mergers, interactions, role of ISM)

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AGN in Clusters of Galaxies

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  1. AGN in Clusters of Galaxies Paul Martini The Ohio State University J.S. Mulchaey, D.D. Kelson (OCIW) E. Kim (CfA), A. Athey (OCIW)

  2. Why Survey Clusters for AGN? Why is this a MISST? • 1. Different environment to probe AGN fueling (mergers, interactions, role of ISM) • 2. Catalysts for galaxy evolution (ram pressure stripping, starvation, etc.) • 3. Feedback of AGN on galaxy ISM and cluster ICM • 4. Source of systematic error for X-ray (and SZ) cluster cosmology surveys • 5. Large population of optically-dull AGN, much higher surface density than blank fields Images from Sun et al. (2005); McNamara et al. (2006); Martini et al. (2002)

  3. AGN Identification We have identified 35 AGN in 8 clusters LMXB relation from Kim & Fabbiano (2004) Hot Gas relation from O’Sullivan et al. (2003) 35 (of 40) X-ray sources are AGN (10x or more X-ray luminous than either LMXBs or hot, gaseous halos) All but 4/35 (filled circles) are optically dull The most luminous contribute ~10% of the cluster LX

  4. AGN Distribution • Radial Distribution • Cumulative AGN and inactive galaxy distributions for all 8 clusters vs. R/r200 • Kinematic Distribution • Distributions vs. |v-vc|/ • Substructure Distribution • Distribution vs.  where • 2 = (11/2) [local - )2 + (local - )2] • (Dressler & Shectman 1988) AGN and inactive galaxies have identical distributions

  5. AC114 (z=0.31) MR = -20 AGN Fraction in Clusters • Cluster AGN Fraction: • The fraction of galaxies brighter than MR = -20 mag with LX>1041 erg/s AGN • fA ~ 5% averaged over 8 clusters • Galaxy population brighter than • MR<-20 mag is the main uncertainty Martini et al. (2006b)

  6. Dependence on Cluster Properties There is good evidence for cluster to cluster variation There are at best ‘intriguing trends’ between AGN fraction and various cluster properties Martini et al. (2006b)

  7. Summary • Cluster AGN fraction is unexpectedly high: fA ~ 5% • Most cluster AGN are optically dull • Cluster AGN trace the cluster galaxy population (to ~0.5 r200) • The AGN fraction varies from cluster to cluster

  8. Wish List for Future Cluster Surveys (The ANEWs of this MISST) • A larger sample to determine if substructure or velocity dispersion influences the AGN fraction in clusters • A high-redshift sample (z>0.5) to determine if there is evolution • Quantification of the impact on cluster cosmology studies • A comparable field AGN fraction

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