Table 1.
Summary of the different strong lensing models.
| Model ID | d.o.f. | Nfree | rms [″] | χ2/d.o.f. |
|---|---|---|---|---|
| Cluster RX J2129 | ||||
| zcluster = 0.234, Nsrc = 7, zsrc = [0.68 − 3.43] | ||||
| R2129 fixed | 22 | 8 | 0.20 | 0.15 |
| R2129 Ωm | 21 | 9 | 0.19 | 0.15 |
| R2129 Ωm, w | 20 | 10 | 0.19 | 0.16 |
| R2129 Ωm, Ωk | 20 | 10 | 0.19 | 0.15 |
| R2129 Ωm, w0, wa | 19 | 11 | 0.19 | 0.16 |
| Cluster Abell S1063 | ||||
| zcluster = 0.348, Nsrc = 20, zsrc = [0.73 − 6.11] | ||||
| A1063 fixed | 56 | 14 | 0.37 | 0.53 |
| A1063 Ωm | 55 | 15 | 0.36 | 0.53 |
| A1063 Ωm, w | 54 | 16 | 0.36 | 0.54 |
| A1063 Ωm, Ωk | 54 | 16 | 0.36 | 0.54 |
| A1063 Ωm, w0, wa | 53 | 17 | 0.36 | 0.54 |
| MACS J1931 | ||||
| zcluster = 0.352, Nsrc = 7, zsrc = [1.18 − 5.34] | ||||
| M1931 fixed | 12 | 12 | 0.38 | 0.91 |
| M1931 Ωm | 11 | 13 | 0.37 | 0.96 |
| M1931 Ωm, w | 10 | 14 | 0.37 | 1.05 |
| M1931 Ωm, Ωk | 10 | 14 | 0.38 | 1.07 |
| M1931 Ωm, w0, wa | 9 | 15 | 0.35 | 1.06 |
| MACS J0329 | ||||
| zcluster = 0.450, Nsrc = 9, zsrc = [1.31 − 6.17] | ||||
| M0329 fixed | 12 | 16 | 0.24 | 0.43 |
| M0329 Ωm | 11 | 17 | 0.23 | 0.46 |
| M0329 Ωm, w | 10 | 18 | 0.21 | 0.40 |
| M0329 Ωm, Ωk | 10 | 18 | 0.23 | 0.50 |
| M0329 Ωm, w0, wa | 9 | 19 | 0.21 | 0.44 |
| MACS J2129 | ||||
| zcluster = 0.587, Nsrc = 11, zsrc = [1.05 − 6.85] | ||||
| M2129 fixed | 40 | 14 | 0.56 | 1.18 |
| M2129 Ωm | 39 | 15 | 0.56 | 1.20 |
| M2129 Ωm, w | 38 | 16 | 0.55 | 1.19 |
| M2129 Ωm, Ωk | 38 | 16 | 0.55 | 1.23 |
| M2129 Ωm, w0, wa | 37 | 17 | 0.55 | 1.31 |
Notes. The columns are the cluster model ID (including the cluster name and the cosmological model), the degrees of freedom (d.o.f.), the number of free parameters (Nfree), the root mean square (rms) of the differences between the observed and model predicted image positions, and the image position χ2 per d.o.f. (i.e., the reduced χ2) for positional uncertainties of 
. For the cosmological model specified in the first column, the listed cosmological parameters indicate the parameters that are allowed to vary. For each cluster we also quote the redshift (zcluster), the number of multiply lensed sources (Nsrc) and their redshift range (zsrc). The models with fixed cosmology assume a flat-ΛCDM scenario with Ωm = 0.3.
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