Table A.1
Constraints on lens parameters for different models of mock cluster lensing mass distribution 1.
| Parameters | Input | MP-full | SP | MP-fore | MP-back | MP-wt |
|---|---|---|---|---|---|---|
θE, fd  |
2.00 |  |
− |  |
− |  |
xhalo  |
0.00 |  |
 |
 |
 |
 |
yhalo  |
0.00 |  |
 |
 |
 |
 |
 |
0.80 |  |
 |
 |
 |
 |
| θhalo [rad] | 0.000 |  |
 |
 |
 |
 |
θE, halo  |
10.00 |  |
 |
 |
 |
 |
rc, halo  |
2.00 |  |
 |
 |
 |
 |
| γhalo | 0.40 |  |
 |
 |
 |
 |
θE, g  |
2.00 |  |
 |
 |
 |
 |
θE, bd  |
2.00 |  |
− | − |  |
 |
rmsbest-fit  |
8 × 10−4 | 0.41 | 0.18 | 0.39 | 0.028 | |
 |
2 × 10−3 | 587 | 116 | 532 | 3 |
Notes.Thefirst column refers to the values used to simulate, the other columns refer to different models, in order, the full multi-plane, the single cluster-plane, the multi-plane with only foreground perturber, the multi-plane with only background perturber and the total multi-plane with the truncation radii of the galaxies fixed to the wrong value (10″ instead of 15″). The values are the medians of the posterior probability distributions of the lens parameters together with their 1σ uncertainties. The orientation is measured counter clockwise from positive x-axis.
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