Table 2
PIEMD parameters inferred for the five dark-matter halos (four large-scale components, one galaxy-scale perturber) considered in the optimization procedure.
| Component | Δ RA | Δ Dec | e | θ | rcore (arcsec) | rs (arcsec) | σ (km s-1) | M (25″) (1012 M⊙) |
|
|
||||||||
| #1 (C) |
|
2.9 |
0.6 ± 0.05 | 70.1 |
7.0 ± 2.7 | [1000] | 857 |
65.5 ± 4.8 |
| #2 (D) | 23.7 |
−22.4 ± 1.6 | > 0.5 | 46.1 ± 7.7 | 5.3 ± 1.7 | [1000] | 535 ± 33 | 27.0 ± 2.5 |
| #3 (B) | 64.2 ± 4.8 | 29.7 ± 3.8 | 0.58 |
159 |
5.0 |
[1000] | 667 |
37.1 ± 7.0 |
| #4 (A) | 111.9 |
63.7 ± 2.0 | >0.55 | 9.0 |
14.9 |
[1000] | 954 ± 74 | 54.3 ± 4.8 |
| L∗ elliptical galaxy | – | – | – | – | [0.02] | 9.1 ± 1.0 | 234 |
– |
Notes. Labels A, B, C and D correspond to the labels given in Fig. 1. Coordinates are given in arcseconds relative to α = 109.3982,δ = 37.745778; e and θ are the ellipticity and position angle of the mass distribution. Error bars correspond to 1σ confidence level. Parameters in brackets are not optimized. The zero point for the scaling relations used to derive the scale radius of the perturbing cluster galaxies is set to a magnitude of 20.66 (F814W band). Letters in parenthesis in Col. 1 denote the four subclusters identified by Ma et al. (2009, see our Fig. 1).
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