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Table B.1.

Lens mass models.

Model Name Description Number of mass parameters Npar χim, MP2
variable with Gaussian priors
iso_halo 25 4 6.3
• primary cluster DM halo: isothermal elliptical mass distribution 6 0
• perturbative cluster DM halo: isothermal elliptical mass distribution 6 0
• cluster members scaling relation for θ E , ∞ ref $ \theta_{\mathrm{E,\infty}}^{\mathrm{ref}} $ and r t ref $ r_{\mathrm{t}}^{\mathrm{ref}} $, with Gaussian prior on velocity dispersion based on Faber-Jackson 2 1
• circular BCG with Gaussian prior on θE, ∞, BCG from velocity-dispersion measurement and uniform prior on rt, BCG 2 1
• cluster member IDphot 116 with Gaussian prior on θE, ∞, 116 from velocity-dispersion measurement and uniform prior on rt, 116 2 1
• three jellyfish galaxies with variable Einstein radii 3 0
• foreground LOS galaxy at zfg = 0.309 with variable θE, ∞, fg and rt, fg 2 0
• background LOS galaxy at zbg = 0.371 with θE, ∞, bg having prior from velocity dispersion and variable rt, bg with uniform prior 2 1
PL_halo 26 4 6.3
• primary cluster DM halo: power-law elliptical mass distribution 7 0
• other components are the same as the iso_halo model above 19 4
NFW_halo 25 4 23
• primary cluster DM halo: elliptical NFW mass distribution 6 0
• other components are the same as the iso_halo model above 19 4
iso_halo+sheet 26 4 6.3
• same components as the iso_halo model above 25 4
• mass-sheet parameter 1 0
iso_halo+ell_BCG 27 4 5.7
• same components as the iso_halo model, excluding the BCG (elliptical instead of circular) 23 3
• elliptical BCG with Gaussian prior on θE, ∞, BCG from velocity-dispersion measurement and uniform priors on rt, BCG, qBCG and ϕBCG 4 1
single_plane 25 4 6.1
• same components as the iso_halo model above except the foreground galaxy (at zfg = 0.309) and background galaxy (at zbg = 0.371) are assumed to be at the cluster redshift of zd = 0.336. The positional uncertainties of the multiple image positions are elliptical, as listed in Table 4 and used in the above models. 25 4
baseline 25 4 7.3
• same components as the single_plane model above except the positional uncertainties of the multiple image positions are circularized from the elliptical uncertainties. The circularized uncertainty is taken to be the geometric mean of the semi-major and semi-minor axis of the elliptical uncertainty ( σ circ = σ major σ minor $ \sigma^{\mathrm{circ}} = \sqrt{\sigma^{\mathrm{major}} \sigma^{\mathrm{minor}}} $). 25 4

Notes. The first line of each model lists the total number of parameters, whereas the subsequent lines indicate the numbers of parameters for the specific components of the mass model. The last column (χim, MP2) is the image-position χ2 of the most-probable mass model. The galaxy mass centroids are located at their observed light centroids, and the galaxies are assumed to be circular, except for the BCG where we considered both circular and elliptical mass distributions. Therefore, all galaxies following the scaling relations are described by two parameters ( θ E , ∞ ref $ \theta_{\mathrm{E,\infty}}^{\mathrm{ref}} $ and r t ref $ r_{\mathrm{t}}^{\mathrm{ref}} $), whereas galaxies not following the scaling relations have each two parameters (θE, ∞, i and rt, i for galaxy i) when they are circular, and four parameters (θE, ∞, BCG, rt, BCG, qBCG and ϕBCG) when elliptical. The number of free parameters for the DM halo parametrizations is described in Sect. 5.1.2 and 5.1.3 and listed in the table.

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