Table 1
Dynamical properties of cluster members L1 and L3.
| Galaxy | L1 | L3 |
|---|---|---|
| ɀ | 0.8722 ± 0.0001 | 0.8642 ± 0.0002 |
| σv,los [kms−1] | 296.1 ± 6.1 | 199.2 ± 10.0 |
| θE,SIS [″], realistic (†) | 1.05 ± 0.05 (⋆) | 0.49 ± 0.05 |
| θE,SIS [″], conservative (†) | 0.86 ± 0.04 (⋆) | 0.45 ± 0.05 |
Notes. All quantities are inferred from VLT/MUSE data only, and correspond to the redshift ɀ, LOS stellar velocity dispersion σv,los and corresponding Einstein radius θE,SIS assuming an SIS mass distribution (Eq. (2)). Uncertainties for redshifts and velocity dispersions contain both statistical and systematic uncertainties, adding in quadrature.(†) The “realistic” and “conservative” cases relate to the estimated contribution of the cluster, described in Sect. 3.2.(⋆) In this work, we infer that the density profile L1 is steeper than for an SIS from lensing constraints (Sect. 5.3).
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