Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data II: Hierarchical Bayesian Modeling of the Red-Sequence Galaxy Luminosity Function

Zhang, Y. and Miller, C. J. and Rooney, P. and Bermeo, A. and Romer, A. K. and Cervantes, C. Vergara and Rykoff, E. S. and Hennig, C. and Das, R. and McKay, T. and Song, J. and Wilcox, H. and Bacon, D. and Bridle, S. L. and Collins, C. and Conselice, C. and Hilton, M. and Hoyle, B. and Kay, S. and Liddle, A. R. and Mann, R. G. and Mehrtens, N. and Mayers, J. and Nichol, R. C. and Sahlén, M. and Stott, J. and Viana, P. T. P. and Wechsler, R. H. and Abbott, T. and Abdalla, F. B. and Allam, S. and Benoit-Lévy, A. and Brooks, D. and Buckley-Geer, E. and Burke, D. L. and Carnero Rosell, A. and Carrasco Kind, M. and Carretero, J. and Castander, F. J. and Crocce, M. and Cunha, C. E. and D'Andrea, C. B. and da Costa, L. N. and Diehl, H. T. and Dietrich, J. P. and Eifler, T. F. and Flaugher, B. and Fosalba, P. and García-Bellido, J. and Gaztanaga, E. (2019) Galaxies in X-ray Selected Clusters and Groups in Dark Energy Survey Data II: Hierarchical Bayesian Modeling of the Red-Sequence Galaxy Luminosity Function. Monthly Notices of the Royal Astronomical Society, 488 (1). pp. 1-17. ISSN 0035-8711

[img]
Text (1710.05908)
1710.05908.pdf - Accepted Version
Available under License Creative Commons Attribution-NonCommercial.

Download (1MB)

Abstract

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 luminosity function simultaneously in redshift (0.1 <z <1.05) and cluster mass (13.5 \le {log_{10}}(M_{200crit}) ˜ <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 Schecter 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% 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.

Item Type:
Journal Article
Journal or Publication Title:
Monthly Notices of the Royal Astronomical Society
Additional Information:
This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. The definitive publisher-authenticated version Y Zhang, C J Miller, P Rooney, A Bermeo, A K Romer, C Vergara Cervantes, E S Rykoff, C Hennig, R Das, T McKay, J Song, H Wilcox, D Bacon, S L Bridle, C Collins, C Conselice, M Hilton, B Hoyle, S Kay, A R Liddle, R G Mann, N Mehrtens, J Mayers, R C Nichol, M Sahlén, J Stott,[et al.] , (DES Collaboration), Galaxies in X-ray selected clusters and groups in Dark Energy Survey data – II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function, Monthly Notices of the Royal Astronomical Society, Volume 488, Issue 1, September 2019, Pages 1–17, https://doi.org/10.1093/mnras/stz1612 is available online at: https://academic.oup.com/mnras/article/488/1/1/5513465
Uncontrolled Keywords:
/dk/atira/pure/subjectarea/asjc/1900/1912
Subjects:
ID Code:
135491
Deposited By:
Deposited On:
22 Jul 2019 14:10
Refereed?:
Yes
Published?:
Published
Last Modified:
19 Sep 2020 05:59