Euclid preparation - LXV. Determining the weak lensing mass accuracy and precision for galaxy clusters

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Volume 695 (March 2025)

A&A, 695 (2025) A280

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Table 3.

Relative change of the WL mass with respect to the ‘LSS plus shape noise’ case due to systematic effects.

Data Set	⟨ΔlnM⟩	ΔlnM_⟨ΔΣ⟩
photo-z non-conservative (Sect. 5.1.1)	−0.080 ± 0.002	−0.223 ± 0.015
photo-z robust (Sect. 5.1.2)	0.000 ± 0.004	0.007 ± 0.017
`AMICO`-like (Sect. 5.2)	−0.015 ± 0.003	0.053 ± 0.017
`PZWav`-like (Sect. 5.2)	−0.025 ± 0.003	0.009 ± 0.015
masks (Sect. 5.3)	0.000 ± 0.002	0.013 ± 0.015
BMO (Sect. 6.1)	0.004 ± 0.001	0.051 ± 0.015
$\begin{matrix} photo- z robust + \\ AMICO -like + \\ masks + (Sect . 7) \\ BMO + prior \end{matrix}$ $\begin{aligned} & \text{ photo-}z \text{ robust}\, +\\ & {\mathtt{AMICO}}\text{-like} \,+ \\ & \text{ masks} + {\quad\quad\quad}(\mathrm{Sect.} 7)\\ & \text{ BMO} + \text{ prior} \end{aligned}$	−0.006 ± 0.006	0.129 ± 0.019

Notes. We consider the ML estimator. Measured quantities are derived from the cluster mass average (⟨ΔlnM⟩), or the cluster lensing profile average (ΔlnM_⟨ΔΣ⟩). Errors are computed as the standard deviation of the bootstrap sample distribution (mass average) and the standard deviation of the marginalised mass posterior distribution, added in quadrature (lensing profile).

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