2020/12/21 by K. Kiiveri, D. Gruen, A. Finoguenov +31 · 15 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Gamma-ray bursts and supernovae #Geometry #Lambda #Physics #ROSAT #Redshift #Scaling #Virial mass #Weak gravitational lensing #astro-ph.CO
paper · pdf · doi:10.1093/mnras/staa3936
published in Monthly Notices of the Royal Astronomical Society 502(1), 1494-1526 (Oxford University Press) · 37 pages, 12 figures
openalex publication_date 2020/12/21 · arxiv created 2021/01/06 · arxiv updated 2021/02/10 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
ABSTRACT The COnstrain Dark Energy with X-ray clusters (CODEX) sample contains the largest flux limited sample of X-ray clusters at 0.35 < z < 0.65. It was selected from ROSAT data in the 10 000 square degrees of overlap with BOSS, mapping a total number of 2770 high-z galaxy clusters. We present here the full results of the CFHT CODEX programme on cluster mass measurement, including a reanalysis of CFHTLS Wide data, with 25 individual lensing-constrained cluster masses. We employ lensfit shape measurement and perform a conservative colour–space selection and weighting of background galaxies. Using the combination of shape noise and an analytic covariance for intrinsic variations of cluster profiles at fixed mass due to large-scale structure, miscentring, and variations in concentration and ellipticity, we determine the likelihood of the observed shear signal as a function of true mass for each cluster. We combine 25 individual cluster mass likelihoods in a Bayesian hierarchical scheme with the inclusion of optical and X-ray selection functions to derive constraints on the slope α, normalization β, and scatter σln λ|μ of our richness–mass scaling relation model in log-space: ⟨ \rm In λ | μ⟩ = αμ + β, with μ = ln (M200c/Mpiv), and Mpiv = 1014.81M⊙. We find a slope α = 0.49+0.20-0.15, normalization exp (β) = 84.0+9.2-14.8, and σ ln λ | μ = 0.17+0.13-0.09 using CFHT richness estimates. In comparison to other weak lensing richness–mass relations, we find the normalization of the richness statistically agreeing with the normalization of other scaling relations from a broad redshift range (0.0 < z < 0.65) and with different cluster selection (X-ray, Sunyaev–Zeldovich, and optical).