Y.-Y. Zhang, C. J. Miller, P. J. Rooney, A. Bermeo, A. K. Romer, E. S. Rykoff, C. Hennig, R. Das, Timothy A. McKay, J. Song, H. Wilcox, D. Bacon, C. A. Collins, C. J. Conselice, M. Hilton, B. Hoyle, S. T. Kay, A. Liddle, R. Mann, N. Mehrtens, J. A. Mayers, R. C. Nichol, M. Sahlén, J. P. Stott, P. T. P. Viana, R. H. Wechsler, T. M. C. Abbott, F. B. Abdalla, S. S. Allam, A. Benoit-Levy, D. H. Brooks, E. Buckley-Geer, D. L. Burke, F. J. Castander, C. E. Cunha, D'Andrea,C. B., H. T. Diehl, J. P. Dietrich, T. F. Eifler, B. Flaugher, P. Fosalba, J. García-Bellido, E. Gaztanaga, D. Gerdes, D. Gruen, R. A. Gruendl, G. Gutierrez, K. Honscheid, D. James, T. Jeltema, K. Kuehn, N. Kuropatkin, M. Lima, H. Lin, M. A. G. Maia, M. March, J. L. Marshall, P. Melchior, R. Miquel, R. Ogando, A. A. Plazas, E. Sanchez, M. Schubnell, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, F. Sobreira, E. Suchyta, M. E. C. Swanson, G. Tarle, A. R. Walker, M. Desort
Using ∼100 X-ray selected clusters in the Dark Energy Survey Science Verification data, we constrain the luminosity function (LF) of cluster red-sequence galaxies as a function of redshift. This is the first homogeneous optical/X-ray sample large enough to constrain the evolution of the LF simultaneously in redshift (0.1 < z < 1.05) and cluster mass (13.5≤log10(M200crit)∼<15.0). We pay particular attention to completeness issues and the detection limit of the galaxy sample. We then apply a hierarchical Bayesian model to fit the cluster galaxy LFs via a Schechter function, including its characteristic break (m*) to a faint end power-law slope (α). Our method enables us to avoid known issues in similar analyses based on stacking or binning the clusters. We find weak and statistically insignificant (∼1.9σ) evolution in the faint end slope α versus redshift. We also find no dependence in α or m* with the X-ray inferred cluster masses. However, the amplitude of the LF as a function of cluster mass is constrained to ∼20 per cent precision. As a by-product of our algorithm, we utilize the correlation between the LF and cluster mass to provide an improved estimate of the individual cluster masses as well as the scatter in true mass given the X-ray inferred masses. This technique can be applied to a larger sample of X-ray or optically selected clusters from the Dark Energy Survey, significantly improving the sensitivity of the analysis.
galaxies: clusters: general; galaxies: evolution
Monthly Notices of the Royal Astronomical Society
Volume 488, Issue 1, Page 1