Table 5.
Best-fit and marginalized values with 1σ uncertainties for model Img-MP (L/D) based on joint constraints from strong lensing and stellar dynamics.
| Component | Parameter | Best-fit | Marginalized |
|---|---|---|---|
| Kinematics | βz | 0.52 |
 |
| cos i | 0.080 |
 |
|
| BGG | rtr, BGG [″] | 15.5 |
 |
| (dPIE) | θE, BGG [″] | 6.8 |
 |
| xGH [″] | 72.8 |
 |
|
| yGH [″] | 63.7 |
 |
|
| Group halo | qGH | 0.81 |
 |
| (SPEMD) | θPA, GH [°] | 131.5 |
 |
| rcore, GH [″] | 7.8 |
 |
|
| θE, GH [″] | 20.4 |
 |
|
| γGH | 0.81 |
 |
|
| rtr, ref [″] | 5.1 |
 |
|
| θE, ref [″] | 0.61 |
 |
|
| Group members | θE, 1 [″] | 1.3 |
 |
| (dPIE) | θE, 2 [″] | 1.5 |
 |
| θE, 6 [″] | 3.1 |
 |
|
| θE, 7 [″] | 1.8 |
 |
|
| S0 (PIEMD) | θE, S0 [″] | 4.6 |
 |
| External | γext | 0.06 |
 |
| Shear | θext [°] | 180.6 |
 |
Notes. We show the anisotropy βz and inclination angle i of the kinematic model, followed by the same list of parameters as in Tables 3 and 4. Img-MP (L/D) assumes the same mass parametrization as our lensing-only models. It is constrained by the positions of multiple images from six different families and by the lens stellar kinematics over 11 Voronoi bins. Due to different implementations in the GLaD and GLEE softwares, we scaled the truncation and Einstein radii of group members with respect to the BGG and to the reference galaxy, respectively, optimizing the parameters rtr, BGG and θE, BGG instead of rtr, ref and θE, ref. This modification does not impact the final results.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.