Publication Date:
2020-09-07
Description:
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 ∼6, 000 clusters split into 12 subsets spanning the ranges 0.1 ≤ z 〈 0.65 and μ⋆ up to ∼5.5 × 1013M⊙, 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 NFW halo profile, halo triaxiality and projection effects. We use the inferred masses to estimate the joint mass–μ⋆–z scaling relation given by $langle M_{200c} | mu _{star },z
angle = M_0 (mu _{star }/5.16imes 10^{12} mathrm{M_{odot }})^{F_{mu _{star }}} ((1+z)/1.35)^{G_z}$. We find M0 = (1.14 ± 0.07) × 1014M⊙ with $F_{mu _{star }}= 0.76 pm 0.06$ and Gz = −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; ii) testing systematics such as projection effects for applications in cluster cosmology.
Print ISSN:
0035-8711
Electronic ISSN:
1365-2966
Topics:
Physics
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