μ* masses: Weak-lensing calibration of the dark energy survey year 1 redMaPPer clusters using stellar masses
We present the weak-lensing mass calibration of the stellar-mass-based μ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time, we are able to perform a calibration of μ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 clusters split into 12...
| Autores: | , , , , , |
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| Formato: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2020 |
| País: | España |
| Recursos: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/237035 |
| Acesso em linha: | http://hdl.handle.net/10261/237035 |
| Access Level: | acceso abierto |
| Palavra-chave: | Cosmology: observations Galaxies: clusters: general Gravitational lensing: weak |
| Resumo: | We present the weak-lensing mass calibration of the stellar-mass-based μ mass proxy for redMaPPer galaxy clusters in the Dark Energy Survey Year 1. For the first time, we are able to perform a calibration of μ at high redshifts, z > 0.33. In a blinded analysis, we use ∼6000 clusters split into 12 subsets spanning the ranges 0.1 ≤ z < 0.65 and μ up to ∼5.5 × 10 M, and infer the average masses of these subsets through modelling of their stacked weak-lensing signal. In our model, we account for the following sources of systematic uncertainty: shear measurement and photometric redshift errors, miscentring, cluster-member contamination of the source sample, deviations from the Navarro-Frenk-White halo profile, halo triaxiality, and projection effects. We use the inferred masses to estimate the joint mass-μz scaling relation given by M|μ, z = M(μ5.16 × 10 M) ((1 + z)/1.35). We find M = (1.14 ± 0.07) × 10 M with F= 0.76 ± 0.06 and G = −1.14 ± 0.37. We discuss the use of μ as a complementary mass proxy to the well-studied richness λ for: (i) exploring the regimes of low z, λ < 20 and high λ, z ∼ 1; and (ii) testing systematics such as projection effects for applications in cluster cosmology. |
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