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  • 1710.05908

    Rights statement: 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

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

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<mark>Journal publication date</mark>1/09/2019
<mark>Journal</mark>Monthly Notices of the Royal Astronomical Society
Issue number1
Volume488
Number of pages17
Pages (from-to)1-17
Publication statusPublished
Early online date10/06/19
Original languageEnglish

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.

Bibliographic note

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