Table 3.
Best-fit and marginalized values with 1σ uncertainties for the parameters of our lensing-only models based on image positions, in the single-plane (Img-SP (L)) and multi-plane scenarios (Img-MP (L)).
Img-SP (L) |
Img-MP (L)* |
||||
---|---|---|---|---|---|
Component | Parameter | Best-fit | Marginalized | Best-fit | Marginalized |
BGG | rtr, BGG [″] | 17.60 |
![]() |
16.28 |
![]() |
(dPIE) | θE, BGG [″] | 7.79 |
![]() |
9.07 |
![]() |
xGH [″] | 71.86 |
![]() |
72.79 |
![]() |
|
yGH [″] | 64.34 |
![]() |
63.24 |
![]() |
|
Group halo | qGH | 0.96 |
![]() |
0.833 |
![]() |
(SPEMD) | θPA, GH [°] | 106.8 |
![]() |
133.9 |
![]() |
rcore, GH [″] | 13.85 |
![]() |
8.65 |
![]() |
|
θE, GH [″] | 24.13 |
![]() |
19.11 |
![]() |
|
γGH | 0.94 |
![]() |
0.79 |
![]() |
|
rtr, ref [″] | 5.86 |
![]() |
5.42 |
![]() |
|
θE, ref [″] | 0.044 |
![]() |
0.44 |
![]() |
|
Group members | θE, 1 [″] | 0.89 |
![]() |
1.66 |
![]() |
(dPIE) | θE, 2 [″] | 0.81 |
![]() |
1.54 |
![]() |
θE, 6 [″] | 1.24 |
![]() |
2.89 |
![]() |
|
θE, 7 [″] | 2.48 |
![]() |
2.09 |
![]() |
|
S0 (PIEMD) | θE, S0 [″] | – | – | 4.36 |
![]() |
External | γext | 0.033 |
![]() |
0.063 |
![]() |
Shear | θext [°] | 190.72 |
![]() |
179.39 |
![]() |
Notes. The parameters listed are the BGG truncation radius rtr, BGG, the BGG Einstein radius θE, BGG, the group halo centroid (xGH, yGH) with respect to the reference coordinates in Fig. 1, the group halo axis ratio qGH, position angle θPA, GH measured counterclockwise from the x-axis, core radius rcore, GH, Einstein radius θE, GH, and density slope γGH, the reference galaxy truncation radius rtr, ref, and Einstein radius θE, ref, the Einstein radius of group members 1, 2, 6, 7, the Einstein radius of S0 θE, S0 for the multi-plane model, the magnitude of the external shear γext, and the shear angle θext measured counterclockwise from the x-axis. The Einstein radii of group members 1, 2, 6, and 7 are fitted separately, while their truncation radius are scaled to the reference galaxy (see text for details). Note that all θE values shown in the table are scaled for sources at redshift z = ∞. To obtain the actual θE for a given source at redshift zs, the displayed θE needs to be multiplied with the respective Dds/Ds.
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