1. X-ray and Radio AGN in Coma Cluster Progenitors Quyen Nguyen Hart University of Colorado at Boulder, Center for Astrophysics and Space Astronomy Collaborators CU-Boulder John Stocke Erica Ellingson Eric Hallman U. Of Michigan Gus Evrard

2. Why should we follow this road? On the Road to Coma More Massive Cluster Less Massive Cluster

3. On the Road to Coma

4. Multi-wavelength Study Chandra Archival data VLA 20-cm maps (new/archival) HST archival images Apache Point Observatory, 3.5m –Two color imaging (g,r) or (r,i) K-short –Med. Dispersion spectrograph with red/blue channels (3500 - 9000 Å) Additional sources –SDSS –ChaMP –CNOC-1 –Literature

5. Example of Data Abell 963, z=0.206 Chandra 0.3-8.0 keV FIRSTSDSS r

6. AGN Luminosity Limits X-ray LF Sazonov & Revnivtsev (2004) 1 order below knee Ledlow & Owen 1996 1.4 GHz - Radio LF 2 orders below knee X-ray0.3-8 keV 3  10 42 erg s -1 Radio20 cm 1  10 23 W Hz 1

7. Passive Galaxy Spectrum Ca HK B-band Na I Mg I APO DIS spec, r ~ 17th A-band G-band APO DIS spec, r ~ 19th

8. Emission-Line Spectrum APO DIS spec, r ~ 18.5th [O II] [Ne V] [Ne III] Ca HK [O III] H-  [N II] [S II] z=0.209

9. Simple Number Counts 12 low-z clusters (0.2 < z < 0.5) Radio Sources (~40) X-ray Point Sources (~60) TWO Radio AGN per Cluster ONE Xray AGN per Cluster

10. Upper/lower limits reached by APO 3.5m spectroscopy M r * ~ 20.8 Composite COLOR MAGNITUDE Diagram Cluster Red Sequence “old, dead, red galaxies”

11. M r * ~ 20.8 X-ray AND Radio AGN With optical counterparts (N ~ 100)

12. Xray AGN Cluster Member Radio AGN Cluster Member Xray AGN Non-member Radio AGN Non-member Redshift unknown Majority of cluster AGN lies on Cluster Red Sequence (CRS) Some X-ray AGN have BLUER colors than CRS; emission-line spectra Host galaxies of Cluster AGN are bright cluster galaxies M r * ~ 20.8

13. AGN Host Galaxies Cluster AGN optical colors representative of old, red, & dead galaxies, ie. Passive ellipticals Spectra reveal that in our sample –X-ray AGN: ~75% passive galaxy host –Radio AGN: ~80% passive galaxy host In both cases, only a ~few AGN would have been identified optically

14. AGN Projected Distance from ICM X-ray Emission Centroid 1 Mpc 750 kpc 500 kpc 250 kpc

15. Xray Radio ALL AGN Cluster Red Sequence Galaxies ICM EMISSION (  - Model) R core 100 kpc 400 kpc Cluster AGN are more centrally concentrated than red sequence galaxies!

16. In Summary Road to Coma is unique sample Majority of cluster AGN reside within 500 kpc –distributed heating in cluster centers? Cluster AGN host galaxies are passive ellipticals (old, red, & dead galaxies!) RARE overlap of X-ray and Radio AGN sources –Different modes of AGN activity?

17. What’s next… AGN population in z>0.5 sample X-ray hardness ratios; composite X-ray spectrum X-ray and Radio luminosity Functions –Is there an X-ray bi-variate luminosity function similar to radio? Input cluster AGN properties in cosmological simulations This research is supported by Chandra Archive/Theory Grant AR8-9013X