1. Weak-Lensing selected, X-ray confirmed Clusters and the AGN closest to them Dara Norman NOAO/CTIO 2006 November 6-8 Boston Collaborators: Deep Lens Survey Team: David Wittman, Tony Tyson, Vera Margoniner - UC Davis, Jack Hughes - Rutgers U., Ian Dellantonio - Brown U. Recent additions: Ilona Soechting - University of Oxford, Percy Gomez - Gemini

2. Motivation Hierarchical structure formation scenarios may provide a framework for: the evolution of galaxy clusters the growth of black holes the triggering of quasar activity There is a wealth of evidence that AGN know about the larger scale environment. The Cluster AGN Environment: Clues to Formation/Evolution

3. Black Holes know about their host galaxies Black hole mass/velocity dispersion show a correlation Black hole mass/velocity dispersion show a correlation e.g. Ferrarese & Merritt, 2000 Gebhardt et al., 2000 Gebhardt et al., 2000 Black Hole Mass (M sun ) Velocity Dispersion ( kms -1 )

4. AGN know about their neighbors Evidence of mergers in host galaxies Evidence of mergers in host galaxies e.g. Hutchings, et al. 2002

5. Quasars know about Large Scale Structure (?) N-body simulations with toy models of quasar formation can re-produce B-band quasar luminosity function N-body simulations with toy models of quasar formation can re-produce B-band quasar luminosity function e.g. Kauffmann & Haehnelt, 2000

6. Survey of AGN in DLS Clusters Main Goals: Determine if AGN triggering and evolution is influenced by the cluster environment. Determine if AGN triggering and evolution is influenced by the cluster environment. Compare the weak lensing, X-ray gas and dynamical mass environments of AGN Compare the weak lensing, X-ray gas and dynamical mass environments of AGN Compare the AGN fraction in DLS clusters to other samples. Compare the AGN fraction in DLS clusters to other samples.

7. Deep Lens Survey Sample of total mass overdensities is selected from the Deep Lens Survey Sample of total mass overdensities is selected from the Deep Lens Survey Five 2º x 2° fields Five 2º x 2° fields 3x3 grid of Mosaic Fields (35’x35’) 3x3 grid of Mosaic Fields (35’x35’) R ~ 26.5 R ~ 26.5 ~50 galaxies/arcmin 2 ~50 galaxies/arcmin 2 BVRz’ imaging BVRz’ imaging Main Survey Goals: Main Survey Goals: Measure cosmic shear due to large scale structures Measure cosmic shear due to large scale structures Measure the cluster mass function to z~1 Measure the cluster mass function to z~1 dls.physics.ucdavis.edu DLS Cluster 3 8’

8. A Unique Cluster Sample The DLS clusters are the only sample of clusters discovered solely by their mass properties through weak gravitational lensing techniques. The DLS clusters are the only sample of clusters discovered solely by their mass properties through weak gravitational lensing techniques. Lensing provides the only way to measure cluster mass that is not dependent on dynamical state. Lensing provides the only way to measure cluster mass that is not dependent on dynamical state. Provides an opportunity to identify young and forming clusters Provides an opportunity to identify young and forming clusters

9. DLS Cluster Sample 20 shear selected mass overdensities discovered to date. 20 shear selected mass overdensities discovered to date. Suggests about 8 clusters per sq. deg. Suggests about 8 clusters per sq. deg. DLS sample of clusters DLS sample of clusters Mass Range = 4x10 13 - 6x10 14 M  and Mass Range = 4x10 13 - 6x10 14 M  and Redshift range of main clusters = 0.19 - 0.68 20’ DLS Clu 2DLS Clu 8 Wittman et al. 2006 ApJ 643 128

10. DLS Clu 2 DLS overdensities are true X-ray clusters 8 have Chandra X-ray data (~20 ks) also taken. 8 have Chandra X-ray data (~20 ks) also taken. Most show evidence of substructure (mass and X-ray), which may indicate merger activity. Most show evidence of substructure (mass and X-ray), which may indicate merger activity. (e.g Motl et al., 2004, Mohr et al., 1993) (e.g Motl et al., 2004, Mohr et al., 1993)

11. Weak lensing discovered, X-ray Confirmed Clusters

12. X-ray point source distribution  Chandra observations also reveal a large number of X- ray point sources in these cluster fields.  These sources appear to show an aversion to the most massive regions of the cluster.  Seen before in optical.  Söchting, et al. (2000, 2004)  Voronoi tesselation technique

13. Field X-ray point sources 123 X-ray point sources with S/N > 2 in 3 cluster fields Limiting flux is ~ 8 x 10 -15 ergs s -1 cm -1 Clusters have redshifts of 0.3, 0.3 and 0.68

14. R-band matches 68 sources match DLS R band sources to 1.5’’ R magnitudes = ~16.2 - 26 Good photmetric redshifts are currently available for 31 sources

15. X-ray point source Surface Density  For all sources in the field X-ray sources show two peaks,  a strong peak in the central 0.25 Mpcs and  a broad peak in surface density at about 1.25 - 1.75 Mpc, true for both z=0.3 and 0.68 clusters.

16. X-ray point source Surface Density Ruderman and Ebeling, 2005 Ruderman & Ebeling,2005 see similar trend for 51 massive clusters in the Massive Cluster Survey. But only for relaxed galaxies.

17. X-ray point source Surface Density Several sources are known to be background. Elimination of these and HR < -0.5 increases surface density in the center but keeps the 1.4 Mpc peak. Are these infall regions where AGN activity is triggered?

18. Need for spectroscopic data for point sources and cluster galaxies   Kinematical studies of the cluster galaxies   At these low redshifts, photo-z errors result in mis-identifications of cluster membership.   Statistical gravitational lensing of background sources can be significant for these lower redshift fields.   Background sources can be brighted into a flux limited sample by lensing.   Angular Correlation measures for Radio and Optical AGN show over densities on scales of 0.7-1.0 Mpc at z=0.3 Models from Dolag and Bartelmann, 1997 Norman & Impey, 2000

19. Future Plans 5 Additional clusters for analysis 5 Additional clusters for analysis More DLS color data is now available for measuring additional photometric redshifts More DLS color data is now available for measuring additional photometric redshifts Applications for 4m time to get redshifts of brighter sources Applications for 4m time to get redshifts of brighter sources 8m time on young merging cluster galaxies for kinematical analysis of these clusters. 8m time on young merging cluster galaxies for kinematical analysis of these clusters. Determine the AGN fraction in young and merging clusters. Determine the AGN fraction in young and merging clusters. Address the possibility of statistical lensing in these clusters. Address the possibility of statistical lensing in these clusters.

20. Summary DLS cluster sample is the ONLY cluster sample selected by weak lensing shear techniques and is not dependent on cluster dynamical state. A large number of identified clusters show X-ray substructure. X-ray point sources in the fields of DLS weak gravitational lensing discovered fields show and aversion to the densest mass distribution as determined by gravitational shear mass maps. Surface density shows peaks in the core and at 1.5 Mpc. Spectroscopic redshifts for X-ray sources are needed in order to eliminate contamination by background sources. An accurate census of cluster (versus background) AGN is essential to the use of their distribution to understand cluster formation and AGN triggering.