Table 4.
Lens and source parameter constraints for the different configurations for our first set of mock data (presented in Sect. 3.1).
| Parameter description | Parameter | Input | Prior | LD (SN20) | LD (SN30) | L | MFL |
|---|---|---|---|---|---|---|---|
| Source | |||||||
| Light | |||||||
| x centroid | xc, s [″] | 4.3325 | (3.,8.) |
 |
 |
 |
 |
| y centroid | yc, s [″] | 3.5139 | (3.,8.) |
 |
 |
 |
 |
| Axis ratio | qs | 0.850 | (0.5,1.) |
 |
 |
 |
 |
| Position angle | θs [radians] | 0.00 | – |
 |
 |
 |
 |
| Intensity | Ie, s [counts] | 180 | (0.,300.) |
 |
 |
 |
 |
| Effective radius | Reff, s [″] | 0.500 | (0.2,2.) |
 |
 |
 |
 |
| Sersic index | ns | 4.0 | (0.5,10.) |
 |
 |
 |
 |
| Mass | |||||||
| Anisotropy | β | −0.15 | (−0.3,0.3) |
 |
 |
 |
 |
| Inclination | i [radians] | 0.10 | (0.,0.2) |
 |
 |
 |
 |
| Mass-to-light ratio |
 |
– | (1.,7.) | – | – | – |
 |
| Axis ratio |
 |
0.90 | (0.5,1.) |
 |
 |
 |
– |
| Einstein radius |
 [″] |
1.15 | (0.,5.) |
 |
 |
 |
– |
| Lens | |||||||
| Light | |||||||
| Axis ratio | ql | 0.768 | (0.2,1.) |
 |
 |
 |
 |
| Intensity | Ie, l [counts] | 965. | (800.,1100.) |
 |
 |
 |
 |
| Effective radius | Reff, l [″] | 0.900 | (0.3,2.) |
 |
 |
 |
 |
| Sersic index | nl | 4.00 | (0.5,10.) |
 |
 |
 |
 |
| Mass | |||||||
| x centroid |
 [″] |
4.4083 | (4.,5.) |
 |
 |
 |
 |
| y centroid |
 [″] |
3.9934 | (3.5,5.5) |
 |
 |
 |
 |
| Axis ratio |
 |
0.808 | (0.2,1.) |
 |
 |
 |
 |
| Position angle |
 [radians] |
3.669 | – |
 |
 |
 |
 |
| Einstein radius |
 [″] |
3.75 | – |
 |
 |
 |
 |
| Slope |
 |
0.471 | (0.2,0.8) |
 |
 |
 |
 |
| Shear strength | γext, ∞ | 0.1892 | (0.,0.3) |
 |
 |
 |
 |
| Shear position angle | ϕext [radians] | 1.596 | (−3.1415,3.1415) |
 |
 |
 |
 |
 |
1.02 | 1.02 | 1.02 | 1.07 | |||
 |
1.1 | 0.95 | 1.63 | ||||
 |
1.02 | 1.02 | 1.02 | 1.07 | |||
Notes. The columns show the best-fitting values with the corresponding 1σ uncertainties for the joint lensing and dynamical models (LD) with different signal-to-noise ratios for the binning (SN20 and SN30), for the lensing-only model (L), and finally for models with a mass-follows-light profile for the source mass distribution (with SN30) to test for systematic uncertainties related to the source mass parameterisation.
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