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We present the first weak-lensing-based scaling relation between galaxy mass, M ₖ₋, ₀₍₃ ₈₍ₓ₄₆ₑ₀ₓ₄₃ ₂₎₌ₓ₎₍ ₀ₑ₀₌₄ₓ₄ₑ ₘ 䂺₇. ₎₁ₒ₄ₑₕ₀ₓ₈₎₍ₒ ₎₅ ₁₈ ₆₀₋₀ₗₘ ₂₋ₔₒₓ₄ₑₒ ₀ₓ ₙ \\~= 0. 2 were with the Subaru 8. 2 m telescope and the Sunyaev-Zel'dovich. The M WL-Y ₛph scaling relations, measured \ = 500, 1000, and 2500 \_ c, are consistent in and normalization with previous results derived under the of hydrostatic equilibrium (HSE). We find an intrinsic in M WL at fixed Y ₛph of 20\\%, larger than previous measurements of M HSE-Y ₛph scatter well as the scatter in true mass at fixed Y ₛph found in. Moreover, the scatter in our lensing-based scaling is morphology dependent, with 30\\%-40\\% larger M WL undisturbed compared to disturbed clusters at the same Y ₛph at r _ 500. Further examination suggests that segregation may be explained by the inability of our spherical lens to faithfully describe the three-dimensional structure of the, in particular, the structure along the line of sight. We find the ellipticity of the brightest cluster galaxy, a proxy for halo, correlates well with the offset in mass from the mean relation, which supports this picture. This provides empirical that line-of-sight projection effects are an important uncertainty in lensing-based scaling relations.
Marrone et al. (Tue,) studied this question.