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Galaxies in X-ray selected clusters and groups in Dark Energy Survey data - II. Hierarchical Bayesian modelling of the red-sequence galaxy luminosity function

Zhang, Y, Miller, CJ, Rooney, P, Bermeo, A, Romer, AK, Cervantes, CV, Rykoff, ES, Hennig, C, Das, R, Mckay, T, Song, J, Wilcox, H, Bacon, D, Bridle, SL, Collins, CA, Conselice, C, Hilton, M, Hoyle, B, Kay, S, Liddle, AR , Mann, RG, Mehrtens, N, Mayers, J, Nichol, RC, Sahlen, M, Stott, J, Viana, PTP, Wechsler, RH, Abbott, T, Abdalla, FB, Allam, S, Benoit-Levy, A, Brooks, D, Buckley-Geer, E, Burke, DL, Carnero Rosell, A, Kind, MC, Carretero, J, Castander, FJ, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Diehl, HT, Dietrich, JP, Eifler, TF, Flaugher, B, Fosalba, P, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lima, M, Lin, H, Maia, MAG, March, M, Marshall, JL, Melchior, P, Menanteau, F, Miquel, R, Ogando, RLC, Plazas, AA, Sanchez, E, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G and Walker, AR (2019) 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, 488 (1). pp. 1-17. ISSN 0035-8711

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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 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.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2019 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: 0201 Astronomical and Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press
Related URLs:
Date Deposited: 05 Feb 2020 11:44
Last Modified: 05 Feb 2020 11:45
DOI or Identification number: 10.1093/mnras/stz1612
URI: http://researchonline.ljmu.ac.uk/id/eprint/12193

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