1. Environmental Dependence of Brightest Cluster Galaxy Evolution Sarah Brough, Liverpool John Moores University Chris Collins, Liverpool John Moores University Doug Burke, Centre for Astrophysics, Harvard Bob Mann, Institute for Astrophysics, Edinburgh Paul Lynam, ESO

2. Introduction Why study BCGs? K-band photometry of BCGs K-band structural properties of BCGs Conclusions

3. Brightest Cluster Galaxies Most luminous galaxies emitting purely photospheric light in the Universe. Found at the centre of clusters and groups of galaxies. Originally studied to determine cosmological parameters (e.g. Sandage et al 1972) and measure large-scale streaming (e.g. Lauer & Postman 1994)

4. Monolithic collapse models predict that these galaxies formed first at very high redshift and have passively evolved since. Hierarchical models predict that these most massive galaxies should have assembled their stellar mass most recently. Therefore, the differences in the predictions of these models should be most apparent in these, most massive galaxies.

5. Aim to examine the evolution of BCGs in host clusters with known X-ray luminosities by studying their physical properties over a wide span of cosmological time. Cluster X-ray luminosity allows an objective, quantitative measure of galaxy environmental density. X-ray selected cluster catalogues: EMSS (Gioia & Luppino 1994); SHARC (Burke et al. 2003); NORAS (Bohringer et al. 2000). Present Study

6. Flux limits of X-ray cluster catalogues Ebeling et al. 2001

7. X-ray luminosity distribution of cluster sample

8. Absolute Magnitudes

9. K-Band Hubble Diagram Brough et al. 2002

10. Inferred Mass of BCGs

11. Difference with environment also observed by Nelson et al. (2002) with Las Campanas Distant Cluster Survey and Ellis & Jones (2004) with 3 X-ray selected clusters. The colour evolution observed by Nelson et al. (2002) is consistent with accretion consisting of old stellar populations.

12. Structural Properties The accretion rates inferred assume that increases in luminosity mean increases in mass. Numerical simulations of dissipationless mergers predict that radii increase, and the surface brightnesses fade (e.g. Navarro 1990, Capelato et al. 1995) Therefore, expect a difference in structural properties with host cluster environment.

13. Petrosian Structural Parameters Measure K-band Petrosian structural parameters. Petrosian Eta(r) = SB(r) - Petrosian parameters are not model dependent, are less affected by zero-point or extinction errors and are more robust than model fits.

14. Correlation with Environment > 99% Significance 95-98% Significance

15. Petrosian Eta Profile Kjaergaard et al. 1993

16. Petrosian Eta Profile Abell 644

17. Conclusions BCGs in high X-ray luminosity clusters assembled their stellar mass at z>1 and have been passively evolving since. BCGs in low X-ray luminosity clusters have assembled more recently and have been undergoing significant mass evolution since z~1. BCG profiles not consistent with those of normal cluster elliptical galaxies.