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Analysis of the weak lensing mass-richness relation of redMaPPer clusters in the LSST DESC DC2 simulations

Feb 12, 2025
26 pages
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Abstract: (arXiv)
Cluster scaling relations are key ingredients in cluster abundance-based cosmological studies. In optical cluster cosmology, weak gravitational lensing has proven to be a powerful tool to constrain the cluster mass-richness relation. This work is conducted as part of the Dark Energy Science Collaboration (DESC), which aims to analyze the Legacy Survey of Space and Time (LSST) of Vera C. Rubin Observatory, starting in 2026. Weak lensing-inferred cluster properties, such as mass, suffer from several sources of bias. In this paper, we aim to test the impact of modeling choices and observational systematics in cluster lensing on the inference of the mass-richness relation. We constrain the mass-richness relation of 3,600 clusters detected by the redMaPPer algorithm in the cosmoDC2 extra-galactic mock catalog (covering 440440 deg2^2) of the LSST DESC DC2 simulation, using number count measurements and stacked weak lensing profiles in several intervals of richness (20≤λ≤20020 \leq \lambda \leq 200) and redshift (0.2≤z≤10.2 \leq z \leq 1). By modeling the mean of the scaling relation as ⟨ln⁡λ∣M200c,z⟩=ln⁡λ0+μzlog⁡[(1+z)/(1+0.5)]+μm[log⁡10(M200c)−14.3]\langle \ln \lambda|M_{\rm 200c}, z\rangle = \ln\lambda_0 + \mu_z\log[(1+z)/(1+0.5)] + \mu_m[\log_{10}(M_{\rm 200c}) - 14.3], our baseline constraints are ln⁡λ0=3.37±0.03\ln\lambda_0 = 3.37\pm 0.03, μz=0.08±0.07\mu_z = 0.08\pm 0.07 and μm=2.18±0.07\mu_m = 2.18 \pm 0.07. We have found that, for a LSST-like source galaxy density, our constraints are robust to a change in concentration-mass relation and dark matter density profile modeling choices, when source redshifts and shapes are perfectly known. We have found that photometric redshift uncertainties can introduce bias at the 1σ1\sigma level, which can be mitigated by an overall correcting factor, fitted jointly with scaling parameters. We find that including positive shear-richness covariance in the fit shifts the results by up to 0.5σ\sigma.
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  • 26 pages, 15 figures, 3 tables, submitted to A&A (abstract shortened for arXiv)